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Institute for Basic Science and Rare Isotope Science Project. Sun Kee Kim. Vision & Objective of IBS. Vision. To be one of the world ’s leading 10 research institutes in basic science. Objective. - PowerPoint PPT Presentation
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Institute for Basic Science and
Rare Isotope Science Project
Sun Kee Kim
Refer to the Special Act of ISBB
To secure creative knowledge and original technology through the worldrsquos leading basic science researchGoal
Nature
President
Independent organization
President of IBS has been appointed by President of Korea for a five-year term
To be one of the worldrsquos leading 10 research institutes in basic science
To become a hub of the worldrsquos basic science research which will lead the advancement of scientific knowledge To train the future leaders of basic science by providing the best possible research environment for young scientists
Vision amp Objective of IBS
1
Vision
Objective
Conducting the worldrsquos top-class research in fields of basic science and pure basic scienceTraining the future leaders of basic scienceBuilding a global network of basic science
Initially Directors are selected without any limit on research themesEarly Stage
Established Stage Research themes are taken into account in the selection of Directors
Key Functions
Research Themes
2 Key Functions
2
rArr Timetable for the implementation of research fields agreed on the appointment of Directors
Creativity
Openness AutonomyIBS
3 Fundamental Principles
Excellence
3
4 Organizational Structure
4
Auditor President Scientific Advisory Board
Secretariats Office of Policy Planning
Office of Research Services
Office of Administrative Services
Research Center(Headquarters)
Research Center(Extramural)
Accelerator Institute(Affiliated Institution)
Board of Directors
Research Center(Campus)
The number of staff 3000 (2017 including visiting scientists and students)
Annual Budget USD 610 million (2017 including operational cost for the Accelerator Institute)
Organization
Rare Isotope Science Project
4 Organizational Structure
5
IBS consists of 50 research centers supporting organizations and affiliated research institutes
- The research centers will be separately located at headquarters (15) campuses (25) and extramural research centers (10) When criteria for excellence are not met the number of research centers for each location may change Campuses KAIST Alliance (10) GIST (5) DGISTUNISTPOSTECH Alliance (10)
IBS Organization
Basic unit of IBS conducting research in the same place - Extramural research centers belong to universities or other research institutes
Individual Research Center
Function
The composition of staff varies depending on research theme and research plan (around 50 staff USD 9 million for annual budget)
- Each center includes a Director around 5 group leaders and support staff Staff
Director is guaranteed autonomy and independence in operating a research centerManage-
ment
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Refer to the Special Act of ISBB
To secure creative knowledge and original technology through the worldrsquos leading basic science researchGoal
Nature
President
Independent organization
President of IBS has been appointed by President of Korea for a five-year term
To be one of the worldrsquos leading 10 research institutes in basic science
To become a hub of the worldrsquos basic science research which will lead the advancement of scientific knowledge To train the future leaders of basic science by providing the best possible research environment for young scientists
Vision amp Objective of IBS
1
Vision
Objective
Conducting the worldrsquos top-class research in fields of basic science and pure basic scienceTraining the future leaders of basic scienceBuilding a global network of basic science
Initially Directors are selected without any limit on research themesEarly Stage
Established Stage Research themes are taken into account in the selection of Directors
Key Functions
Research Themes
2 Key Functions
2
rArr Timetable for the implementation of research fields agreed on the appointment of Directors
Creativity
Openness AutonomyIBS
3 Fundamental Principles
Excellence
3
4 Organizational Structure
4
Auditor President Scientific Advisory Board
Secretariats Office of Policy Planning
Office of Research Services
Office of Administrative Services
Research Center(Headquarters)
Research Center(Extramural)
Accelerator Institute(Affiliated Institution)
Board of Directors
Research Center(Campus)
The number of staff 3000 (2017 including visiting scientists and students)
Annual Budget USD 610 million (2017 including operational cost for the Accelerator Institute)
Organization
Rare Isotope Science Project
4 Organizational Structure
5
IBS consists of 50 research centers supporting organizations and affiliated research institutes
- The research centers will be separately located at headquarters (15) campuses (25) and extramural research centers (10) When criteria for excellence are not met the number of research centers for each location may change Campuses KAIST Alliance (10) GIST (5) DGISTUNISTPOSTECH Alliance (10)
IBS Organization
Basic unit of IBS conducting research in the same place - Extramural research centers belong to universities or other research institutes
Individual Research Center
Function
The composition of staff varies depending on research theme and research plan (around 50 staff USD 9 million for annual budget)
- Each center includes a Director around 5 group leaders and support staff Staff
Director is guaranteed autonomy and independence in operating a research centerManage-
ment
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Conducting the worldrsquos top-class research in fields of basic science and pure basic scienceTraining the future leaders of basic scienceBuilding a global network of basic science
Initially Directors are selected without any limit on research themesEarly Stage
Established Stage Research themes are taken into account in the selection of Directors
Key Functions
Research Themes
2 Key Functions
2
rArr Timetable for the implementation of research fields agreed on the appointment of Directors
Creativity
Openness AutonomyIBS
3 Fundamental Principles
Excellence
3
4 Organizational Structure
4
Auditor President Scientific Advisory Board
Secretariats Office of Policy Planning
Office of Research Services
Office of Administrative Services
Research Center(Headquarters)
Research Center(Extramural)
Accelerator Institute(Affiliated Institution)
Board of Directors
Research Center(Campus)
The number of staff 3000 (2017 including visiting scientists and students)
Annual Budget USD 610 million (2017 including operational cost for the Accelerator Institute)
Organization
Rare Isotope Science Project
4 Organizational Structure
5
IBS consists of 50 research centers supporting organizations and affiliated research institutes
- The research centers will be separately located at headquarters (15) campuses (25) and extramural research centers (10) When criteria for excellence are not met the number of research centers for each location may change Campuses KAIST Alliance (10) GIST (5) DGISTUNISTPOSTECH Alliance (10)
IBS Organization
Basic unit of IBS conducting research in the same place - Extramural research centers belong to universities or other research institutes
Individual Research Center
Function
The composition of staff varies depending on research theme and research plan (around 50 staff USD 9 million for annual budget)
- Each center includes a Director around 5 group leaders and support staff Staff
Director is guaranteed autonomy and independence in operating a research centerManage-
ment
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Creativity
Openness AutonomyIBS
3 Fundamental Principles
Excellence
3
4 Organizational Structure
4
Auditor President Scientific Advisory Board
Secretariats Office of Policy Planning
Office of Research Services
Office of Administrative Services
Research Center(Headquarters)
Research Center(Extramural)
Accelerator Institute(Affiliated Institution)
Board of Directors
Research Center(Campus)
The number of staff 3000 (2017 including visiting scientists and students)
Annual Budget USD 610 million (2017 including operational cost for the Accelerator Institute)
Organization
Rare Isotope Science Project
4 Organizational Structure
5
IBS consists of 50 research centers supporting organizations and affiliated research institutes
- The research centers will be separately located at headquarters (15) campuses (25) and extramural research centers (10) When criteria for excellence are not met the number of research centers for each location may change Campuses KAIST Alliance (10) GIST (5) DGISTUNISTPOSTECH Alliance (10)
IBS Organization
Basic unit of IBS conducting research in the same place - Extramural research centers belong to universities or other research institutes
Individual Research Center
Function
The composition of staff varies depending on research theme and research plan (around 50 staff USD 9 million for annual budget)
- Each center includes a Director around 5 group leaders and support staff Staff
Director is guaranteed autonomy and independence in operating a research centerManage-
ment
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
4 Organizational Structure
4
Auditor President Scientific Advisory Board
Secretariats Office of Policy Planning
Office of Research Services
Office of Administrative Services
Research Center(Headquarters)
Research Center(Extramural)
Accelerator Institute(Affiliated Institution)
Board of Directors
Research Center(Campus)
The number of staff 3000 (2017 including visiting scientists and students)
Annual Budget USD 610 million (2017 including operational cost for the Accelerator Institute)
Organization
Rare Isotope Science Project
4 Organizational Structure
5
IBS consists of 50 research centers supporting organizations and affiliated research institutes
- The research centers will be separately located at headquarters (15) campuses (25) and extramural research centers (10) When criteria for excellence are not met the number of research centers for each location may change Campuses KAIST Alliance (10) GIST (5) DGISTUNISTPOSTECH Alliance (10)
IBS Organization
Basic unit of IBS conducting research in the same place - Extramural research centers belong to universities or other research institutes
Individual Research Center
Function
The composition of staff varies depending on research theme and research plan (around 50 staff USD 9 million for annual budget)
- Each center includes a Director around 5 group leaders and support staff Staff
Director is guaranteed autonomy and independence in operating a research centerManage-
ment
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
4 Organizational Structure
5
IBS consists of 50 research centers supporting organizations and affiliated research institutes
- The research centers will be separately located at headquarters (15) campuses (25) and extramural research centers (10) When criteria for excellence are not met the number of research centers for each location may change Campuses KAIST Alliance (10) GIST (5) DGISTUNISTPOSTECH Alliance (10)
IBS Organization
Basic unit of IBS conducting research in the same place - Extramural research centers belong to universities or other research institutes
Individual Research Center
Function
The composition of staff varies depending on research theme and research plan (around 50 staff USD 9 million for annual budget)
- Each center includes a Director around 5 group leaders and support staff Staff
Director is guaranteed autonomy and independence in operating a research centerManage-
ment
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Selection of Directors
5 Selection amp Management of Research Cen-ters
Scientists fully committed to managing research centers and conducting research over the long termScientists with world renowned research achievements or the potential to do so Scientists capable of carrying out and managing large-scale research projects
Requirements
Excellence of candidates will be a top priority while creativity and superiority of research plan will also be considered
Criteria of Selection
7
It evaluates the selection of Directors and their output on a 3 year basisPresident appoints 15 scholars in various research fields from both at home and abroad
Selection and Evaluation Committee (SEC)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Evaluation Prior evaluation (SEC)Panel review (Subcommittee)Comprehensive evaluation (SEC)
SEC(Subcommitt
ee)
후보자 결정 자문Final review amp consultation SAB
Pre-Selection Selection of Director President
Negotiations Negotiation over research plan bw President and Director Research topics budget period compensation etc
President
Recruitment President
Confirmation Confirmation and appointment of Director President
8
PresidentPlanning Establishing a selection plan of research centers (with consultation from SAB)
Step
Consultation
5 Selection amp Management of Research Cen-ters
Invitation Scouting By
Year-round recruitmentCandidate scouting through SAB
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Staff Management
Directors have discretion in hiring scientists and staff within the budget of research centers
9
5 Selection amp Management of Research Cen-ters
Employment Positions
Directors and group leaders Tenured at IBS or Professors permanent
employees at lsquopartner institutionsrsquo Universities government-invested institutes which signed research centerrsquos employment agreement with partner campuses host institutions or IBS through MOU
As a rule Directors and group leaders work full time
Open-door employment policy with a free flow of renowned scientists and young scientists
- Dispatched workers from other institutions post-doc grad students and visiting scientists
Directors and group leaders should work full time to concentrate on research
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Research budget for each research center is allocated under the three-year plan
5 Selection amp Management of Research Cen-ters
Budget Management
Research output is evaluated on a 3 year basis Output evaluation begins 5 years after the formation of the research centers
(preliminary consultation after the first 2 years)
Results of output evaluation are used in determining research budgets and research topics for the next 3 years
Evaluation of Research Center
10
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
6 Buildings
Buildings
Temporary headquarters is currently in the Daeduk District with offices for research and administration IBS will construct its own headquarter buildings and 3 campuses (including amenities for overseas scientists)Master plan of construction will be established by May 2012 and the construction is scheduled to be completed by the end of 2015 Each campus uses spaces of the universities which host IBS campuses
11
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
7 Main Schedules
12
Establishment of IBS (Prof Se-jung Oh appointed as Founding President)
Invitation Announcement for Directors
IBS Opening Ceremony amp International Symposiums
Opening of The 1st Research Center
Nov 2011
Jan ~ Feb 2012
May 2012
Mid of 2012
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Science Business Belt
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Concept of the Accelerator ComplexIF Linac
Future Extension200 MeVu (U) 8 pμA
Stripper18 MeVu
280 MHz SCL 70 MHzRFQ 70 MHz SCL
28 GHz SC ECR ISH2
+ D+
Spallation Fission Target
RF Cooler
Mass Separator
ISOL Linac
ECR IS
70 MHz SCL 70 MHz RFQ
Charge Breeder
10 keVu
Nuclear Data
Low Energy Experiments
03 MeVu1~5 MeVu18 MeVuHigh Energy Experiments
μSR
MedicalResearch
400 kWTarget
FragmentSeparator
Atomic Trap Experiments
70 kW Cyclotron
GasCatcherGas cell
MaterialScience Beta-NMR
U33+
Nuclear AstrophysicsMaterial scienceBio scienceMedical scienceNuclear data
Atomic Nu-clear physics
Nuclear Physics
Medical sci-ence
Material sci-ence
Material sci-ence
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
16Rare Isotope Factory High intensity RI beams by ISOL amp IFF
70kW ISOL from direct fission of 238U induced by 70MeV 1mA p400kW IFF by 200MeVu 8pμA 238U
High energy high intensity amp high quality neutron-rich RI beams132Sn with up to ~250MeVu up to 9x108 pps
More exotic RI beams by ISOL+IFF+ISOL(trap)
Simultaneous operation modes for the maximum use of the facility
ISOL(Isotope Separator On-Line) p thick target (eg Uranium Carbide) fission fragments rare isotopes
IF(In-Flight Fragmentation) Heavy ion beam thin target projectile fragmentation high energy RI beam or stopping and reacceleration
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
YITP-KoRIA Workshop 17
RI from ISOL by Cyclotron
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
3 ISOL IFF ISOL (trap)
1 ISOL low E RI
2 ISOL high E RI
1
2ISOL with cyclotron driver (70 kW)
3
High energy experiments
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
YITP-KoRIA Workshop 18
RI from IFF by High-Power SC LINACand High-Intensity Stable HI beams
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
200 MeVu (U)
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
4
56 7
6 IFF high E RI
7 High E stable heavy ions
4 Low E stable heavy ions
5 IFF low E RI or ISOL (trap)
Stable HI beamsIFF with stable heavy ions High energy
experiments
175 MeVu (U) gt 11 pμA
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
YITP-KoRIA Workshop 19
RI from ISOL by High-Power SC LINAC(Long term future upgrade option)
November 10-12 2011
LINAC
Experimental Hall
Beam line [for accelera-tion]Beam line [for experi-ment]Target building
IFF LINAC
ISOL LINAC
Future plan
600 MeV 660 mA protons
Stripper
SC ECR IS
CyclotronK~100
Fragment Separator
ChargeBreeder
SCL RFQ
RFQ
SCL
SCL
Low energy experiments
ISOLtarget
In-flighttarget
μ Medi-cal
research
Atom trap
experi-ment
H2+D+
Nuclear AstrophysicsMaterial scienceBio scienceNuclear data
Atomic Nu-clear physics
Medical sci-ence
Nuclear Physics
Future extension area
8 High power ISOL
ISOL with IFF LINAC - future high-power
driver- 400 kW (or ~MW)
ISOL upgrade
8
High energy experiments
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
20
Ion Species Z A
Ion source output SC linac output
Charge Current (pmicroA) Charge Current
(pmicroA)Energy (MeVu)
Power (kW)
Proton 1 1 1 660 1 660 610 400Ar 18 40 8 421 18 337 300 400Kr 36 86 14 221 34-36 175 265 400Xe 54 136 18 186 47-51 125 235 400U 92 238 33-34 117 77-81 84 200 400
IFF Linac Beam Specification
Isotope Half-life Yield at target (pps) Overall eff () Expected Intensity (pps)78Zn 15 s 275 x 1010 00384 11 x 107
94Kr 02 s 744 x 1011 0512 38 x 109
97Rb 170 ms 700 x 1011 088 62 x 109
124Cd 124 s 140 x 1012 002 28 x 108
132Sn 40 s 468 x 1011 0192 90 x 108
133In 180 ms 115 x 1010 0184 21 x 107
142Xe 122 s 511 x 1011 208 11 x 1010
Estimated RIBs based on ISOL
Calculated by Dr B H Kang (Hanyang Univ) for proton beams of 70 MeV and 1 mA with 3 cm thick UC2 target of 25 gcm3
Estimated by KAPRA
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Comparison to other facilities 1Facility Korea
FAIRGSI
Germany
FRIBMSUUSA
RIBFRIKENJapan
RI beam production ISOL+IFF+ISOL(trap) IFF IFF+ISOL ＋ IFF+ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV p 200 MeVu 238U
27 (238U) ~30 (1H) GeVu
~600 MeV p~200 MeVu 238U
Heavy ion440-345 MeVu
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 04 - 15 GeVu of all masses
Catcher-reaccelera-tion 3 12 MeVuIFF ~150 MeVu
lt 345 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics us-ing trapping
bull Nuclear structurebull Antiprotonbull Nuclear matterbull Plasma bull Atomic physics
bull Nuclear structurebull Nuclear astrophysicsbull Fundamental inter-action and symmetry
bull Nuclear structurebull Nuclear reactionbull Nuclear astrophysicsbull Atomic physicsbull Molecular physicsbull Nuclear chemistry
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Medical application
Completion ~2017 2016 ~2017 ~2010
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Planned+ Option
21
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Facility KoreaHIE-ISOLDE
CERNSwiss (EU)
ISAC IIITRIUMFCanada
SPIRAL2GANILFrance
SPESINFNItly
RI beam production
ISOL+IFF+ISOL(trap) ISOL ISOL ISOL ISOL
Beam en-ergy of RI
driver
ISOL 70 MeV p
IFF 600 MeV 1H 200 MeVu 238U
H (~14 GeV) H (~500 MeVu)E (50 MeV)
H (~33 MeV)D (~40 MeV)HI (~145 MeVu)
H (40-50MeV)
RI beam energy
ISOL ~250 MeVu
IFF ~150 MeVu 3-10 MeVu
ISAC I ~18 MeVuISAC II ~16 MeVu
2-25 MeVu 10 MeVu
Basic sci-ence
bull Nuclear structurebull Nuclear astro-physics and syn-thesis
bull Nuclear matter and symmetry energy
bull Atomic physics using trapping
bull Nuclear struc-ture
bull Atomic physicsbull Nuclear astro-physics
bull Fundamental interaction
bull Solid state physics
bull Nuclear struc-ture
bull Nuclear astro-physics
bull Fundamental interaction and symmetry
bull Nuclear physics
bull Condensed matter physics
bull Chemical ef -fects of radi-ation
bull Nuclear structurebull Low energy nu-clear reaction
bull Nuclear astro-physics
bull High T nuclear matter
bull Atom trap for Nuclear physics
Applied science
bull Medical and Biobull Material research bull Nuclear data
bull Bio science bull Radiation bi-ology
Completion ~2017 2015 ~2015 ~2013 2012
ISOL Isotope Source On LineIFF In-flight fragmenta-tion
Comparison to other facilities 2 22
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Research Topics
23
Nuclear Physics Exotic nuclei near the neutron drip line Superheavy Elements (SHE) Equation-of-state (EoS) of nuclear mat-
ter Nuclear Astrophysics
Origin of nuclei Paths of nucleosynthesis Neutron stars and super-
novae Nuclear data with fast neu-
trons Basic nuclear reaction data for fu-
ture nuclear energy Nuclear waste transmutation
Atomic physics Atomic trap Fundamental symmetries
Origin of ElementsStellar Evolution
Application of Rare Isotopes
Material science Production amp Characterization of new
materials -NMR mSR Medical and Bio sci-
ences Advanced therapy technol-
ogy Mutation of DNA New isotopes for medical
imaging
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
- Design of the experimental facilities in conceptual level- User training program with the international collaboration
KoRIA user community
Nuclear Structure
Nuclear Matter
Nuclear Astrophysics
Atomic physics Nuclear data by fast neu-
trons
Material science
Medical and Bio sciences
Facilities for the scientific researches
Large Acceptance Multi-Purpose Spectrometer (LAMPS)
KoRIA Recoil Spectrometer (KRS)
Atom amp Ion Trap System
neutron Time-of-Flight (n-ToF)Β-NMRNQRElastic Recoil Detection (ERD)Laser Selective IonizerHeavy Ion TherapyIrradiation Facility
24
Multi-Purpose Spectrometer
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
r-process
Production of more-exotic medium mass n-rich RI
LISE++ calculationbull EPAX2 modelbull dp p = 223bull Target thickness and beam line parameters
are optimized for each nuclide
N =82
N =50
Z = 28
Z =50
nuclide Estimated Intensity (pps)
110Y 18110Zr 18114Nb 11116Mo 38118Tc 14
Korea RI Accelerator could reach new n-rich isotope with rates of 10-3-10 pps
142Xe (ISOL) post-accelerator re-accelerator In-flight target Fragmentation separator experi-ments
Note that ~103 times higher than 136Xe (350 MeVu 10 pnA)+Be
26
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
27
KoRIA user community
Facility
Nuclear astrophysicsKoRIA Recoil Spectrometer
(KRS)
RMS mode(recoil mass separator)
IRIS mode(In-flight RI separator)
BT mode(beam trans-port)
Main purpose bull direct measurements of capture reaction (pg) and (ag)
bull in-flight RI beam separation using stable or RI beam from KoRIA + spec-trometer
bull production of more exotic beams
bull beam trans-port from Ko-RIA to the fo-cal plane of KRS
Requirements bull background reduction bull high mass resolution (MDM)
bull large angular acceptancebull highly efficient detection system
bull large angular acceptancebull high-density production target sys-tem
bull high-quality beam (high purity low emittance high intensity)
bull 100 transport efficiency
ConfigurationLength ~25 m Space 20 X 5 m2
1) 4 dipole magnets 2) 20 quadruple magnets 3) 4 hexapole magnets 4) velocity filter (Wien filter)
Beam transport system with performance of high efficient high selective and
high resolution spectrometer
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
28Facility
Nuclear astrophysicsTarget System Particle Detection at F3 amp F5
Gamma-ray Detection at F0 amp F5 Front-end electronics
105 Channels gt 2 GHz high frequency
DAQ
ε~ 20 2 MeV γ-ray
Position resolution lt 1 mm
50 keV (FWHM) 5 MeV α-particle
PID for low-energy recoil particle
MCP PPAC amp MWPC
Multiple scattering ~01 mrad ~005 mrad
Counting rate gt 1 MHz gt 2MHz
Beam Tracking at F0 amp F3
Energy loss lt 1 MeVSupersonic jet gas target devel-oped in GSI
LaBr3(Ce)
DGSD
SCGD
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Nuclear collision ex-periment with 132Sn of
~250 MeV per nucleon
bullDipole acceptance ge 50mSr
bullDipole length =10 m bullTOF length ~80 m
Conceptual Design of LAMPS(high energy)
Dipole magnet We can also con-sider the large aperture supercon-ducting dipole magnet (SAMURAI type)
For B=15 T pZ asymp 15 GeVc at 30o
For B=15 T pZ asymp 035 GeVc at 110o
Neutron-detector array
Low pZ
High pZ
Sole-noid
magnet
Science Goal using isototpes with high NZ at high energy for
Nuclear structure Nuclear EOS
Symmetry energyEX Nuclear collision of 132Sn of ~250 MeVu
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
30
Simulated Event DisplayIQMD for Au+Au at 250A MeV
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
Status and Plan
bull Conceptual Design report (Mar 2010 - Feb 2011)
bull IAC review (Jul 2011 ndash Oct 2011)
bull Rare Isotope Science Project started in IBS (Dec 2011)
bull Technical Design Report (by Jun 2013)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
기본계획 ( 안 ) 파일의 그림
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
bull Breakout reaction from hot-CNO to rp-process in stellar explosion such as in binary system (novae and X-ray bursts)
bull Challenges- for direct measurement we need beam intensity gt 1011 pps target density gt 1018 atomscm2 recoil detection efficiency gt 40 then ~1countshr
Reaction rate of 15O(ag)19Ne by indirect methods
PRL 98 242503 (2007)
uncertain
15O(ag)19Ne
bull No direct measurement has been made before
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
One of key Reactions related to 44Ti (Cosmic gamma-ray source) issue but still very uncertain
44Ti is the first unstable nucleus on the a-line and feeds one of minor Ca isotopes 44Ca by beta-decays ie 44Ti (+)44Sc(+)44Ca (1157MeV ndashg ray)
Based on the model more plausible source of 44Ti is the core collapse supernova especially the mass cut region near core but no observations have been presented so far
Question our knowledge on the condition of C-C supernova is certain
Reduction of uncertainty of nuclear physical measurements on several key reactions related to 44Ti production under C-C supernova condition should be needed to confirm our model
45V(p g)46Cr
Very important constraint on building up Core-collapse supernova model
Key reactions 3a process 40Ca(a g)44Ti 44Ti(a p)47V 45V(p g)46Cr
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
YITP-KoRIA Workshop 38November 10-12 2011
18
B-A Li L-W Chen amp CM Ko Physics Report 464 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδEρE
δOδρEρρEρρE
pnpn
sym
sympnpn
)()( with
)()(21)(
)()()()(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)( pn ρρE
2)( δρEsym
E (M
eV)
r (fm-3)
CDR FAIR (2001)
F de Jong amp H Lenske RPC 57 3099 (1998)F Hofman CM Keil amp H Lenske PRC 64 034314 (2001)
![The 30MeV Stage of the ARIEL e-linac - CERNARIEL [1,2] (the Advanced Rare IsotopE Laboratory) is a decade-long project with the objective to provide three simultaneous rare isotope](https://img.dokumen.tips/doc/110x75/6109f3cd6ae3842b1b361329/the-30mev-stage-of-the-ariel-e-linac-cern-ariel-12-the-advanced-rare-isotope.jpg)
