New space and solar weather results obtained by R3DE instrument on EuTEF platform of ISS in 2008

New space and solar weather results New space and solar weather results obtained by R3DE instrument on EuTEF obtained by R3DE instrument on EuTEF

platform of ISS in 2008platform of ISS in 2008

Ts. Dachev Ts. Dachev 11, B. Tomov, B. Tomov11, Pl. Dimitrov, Pl. Dimitrov11, Yu. Matviichuk, Yu. Matviichuk11

DD..-P. -P. HäderHäder2 2 ,, G. HorneckG. Horneck33 and G. Reitz and G. Reitz33

11Solar-Terrestrial Influences Laboratory, Sofia, Bulgaria, Solar-Terrestrial Influences Laboratory, Sofia, Bulgaria, [email protected]ät, Institut für Botanik und Pharmazeutische Biologie, Friedrich-Alexander-Universität, Institut für Botanik und Pharmazeutische Biologie,

Erlangen, Germany Erlangen, Germany [email protected], Institute of Aerospace Medicine, Koln, Germany DLR, Institute of Aerospace Medicine, Koln, Germany [email protected], ,

[email protected]

New results...New results... ESWW5, Brussels, Belgium, 20 Nov. 2008ESWW5, Brussels, Belgium, 20 Nov. 2008 22

OutlookOutlook

InstrumentationInstrumentation Long-term GCR variationsLong-term GCR variations First observation of Relativistic Electrons First observation of Relativistic Electrons

Precipitation at ISSPrecipitation at ISS Characterization of the radiation environment by Characterization of the radiation environment by

the shape and slope of the spectrathe shape and slope of the spectra Asymmetries in SAA dose distributionAsymmetries in SAA dose distribution ConclusionsConclusions

http://www.bas.bg/


InstrumentationInstrumentation The EXPOSE facility supports long term in situ The EXPOSE facility supports long term in situ

studies of microbes in artificial meteorites as well as of microbial communities studies of microbes in artificial meteorites as well as of microbial communities

from special ecological niches, such as endolithic and endoevaporitic from special ecological niches, such as endolithic and endoevaporitic

ecosystems. EXPOSE is mounted on the European Technology Exposure ecosystems. EXPOSE is mounted on the European Technology Exposure

Facility (EuTEF) located on the external plate of Columbus laboratory of Facility (EuTEF) located on the external plate of Columbus laboratory of

International Space Station (ISS). The Radiation Risks Radiometer-Dosimeter International Space Station (ISS). The Radiation Risks Radiometer-Dosimeter

(for European EXPOSE facility) (R3DE) inside the EXPOSE facility is an active, (for European EXPOSE facility) (R3DE) inside the EXPOSE facility is an active,

low mass and small dimensions device, which measure solar radiation in 4 low mass and small dimensions device, which measure solar radiation in 4

channels and space ionizing radiation. The four-channel: UV-A (315-400 nm), channels and space ionizing radiation. The four-channel: UV-A (315-400 nm),

UV-B (280-315 nm), UV-C (<280 nm) and Photosynthetic Active Radiation (PAR) UV-B (280-315 nm), UV-C (<280 nm) and Photosynthetic Active Radiation (PAR)

(400-700 nm) filter dosimeter measure the solar UV irradiance in W/m(400-700 nm) filter dosimeter measure the solar UV irradiance in W/m22. The . The

deposited energy spectra of the space ionizing radiation are measured by a deposited energy spectra of the space ionizing radiation are measured by a

Liulin type 256-channel spectrometer. The analysis of the spectra gives the total Liulin type 256-channel spectrometer. The analysis of the spectra gives the total

dose in dose in Gy.hourGy.hour-1-1 and the particle flux in cm and the particle flux in cm22.s.s-1-1. Measurements of the UV and . Measurements of the UV and

ionizing radiation parameters have 10 second time resolution and are ionizing radiation parameters have 10 second time resolution and are

transmitted by the ISS telemetry system to the ground since 20th of February transmitted by the ISS telemetry system to the ground since 20th of February

2008.2008.

http://www.bas.bg/


R3DE instrument, which is apart of the EXPOSE facility is R3DE instrument, which is apart of the EXPOSE facility is working continuously on the EuTEF platform of Columbus working continuously on the EuTEF platform of Columbus

module on International space station since February 20module on International space station since February 20 thth 2008 2008

R3DER3DE

EuTEFEuTEF

EXPOSEEXPOSE

+Z+Z

A close-up view of the Columbus A close-up view of the Columbus laboratorylaboratory

Credits: ESA/NASACredits: ESA/NASA

The detector of R3DE instrument The detector of R3DE instrument is shielded by less than is shielded by less than 0.4 0.4

g/cmg/cm22 material including: 1 mm material including: 1 mm aluminum + 0.1 mm cuprum +0.2 aluminum + 0.1 mm cuprum +0.2

mm plastic. This allows direct mm plastic. This allows direct hits on the detector by electrons hits on the detector by electrons with energies higher than with energies higher than 0.78, 0.78, MeVMeV and protons with energies and protons with energies

higher than higher than 15.815.8 MeV MeV

http://www.bas.bg/


The R3DE is an active, low mass The R3DE is an active, low mass (120 g)(120 g) and small consumption and small consumption (150 mW)(150 mW) device, which measure solar radiation in 4 channels and space ionizing radiation device, which measure solar radiation in 4 channels and space ionizing radiation in 256 channels. Measurements have 10 s. time resolution and are transmitted in 256 channels. Measurements have 10 s. time resolution and are transmitted

by the ISS telemetry system to the ground since 20th of February 2008 by the ISS telemetry system to the ground since 20th of February 2008

Charge sensitive preamplifier A225

Discriminator

12 bit Analog to digital

converter

SlaveMicro-

controller

Master Micro-controller

12 bit ADC

RS422

SRAM 512 b

Silicon Detector2 cm2 ; 0.3 mm

UV-BPhoto

Diode and Filter

Amplifier shaper

UV-APhoto

Diode and Filter

Amplifier shaper

Amplifier shaper

UV-CPhoto

Diode and Filter

PARPhoto

Diode and Filter

Amplifier shaper

Temperaturesensor

Amplifier

EXPOSE

Faci-lity

+12 V DC

http://www.bas.bg/


R3D-B2/B3 instruments for ESA Biopan 5/6 facilities were successfully flown R3D-B2/B3 instruments for ESA Biopan 5/6 facilities were successfully flown outside of Foton M2/M3 satellites in June 2005 and September 2007. The outside of Foton M2/M3 satellites in June 2005 and September 2007. The

spectrometers are mutually developed with Prof. D.-P. Haeder, University of spectrometers are mutually developed with Prof. D.-P. Haeder, University of Erlangen, Germany Erlangen, Germany

PAR channel

UV-A channel

UV-B channel

UV-C channel

Detector of 256 ChannelsLET spectrometer

SizeSize: : 8282x57x25 mmx57x25 mmWeightWeight: 1: 1229 9 gg

ConsumptionConsumption: : 8484 mWmWFlash memory: 2 MBFlash memory: 2 MB

4 Channels UV spectrometer

http://www.bas.bg/


Long-term GCR variations obtained by comparison of doses Long-term GCR variations obtained by comparison of doses obtained on different satellites Oulu neutron monitor data obtained on different satellites Oulu neutron monitor data

Fo

ton

M2

Fo

ton

M3

ISS IS

S

6.14 6.14 Gy/hGy/h14.6 14.6 Sv/hSv/h

7.38 7.38 Gy/hGy/h16 16 Sv/hSv/h

10.3 10.3 Gy/hGy/h27.2 27.2 Sv/hSv/h

12 12 Gy/hGy/h29.4 29.4 Sv/hSv/h

Solar minimum GCR doses in low earth orbit rise twice during the solar Solar minimum GCR doses in low earth orbit rise twice during the solar maximum, while neutron component on Earth surface rise up only with 10%maximum, while neutron component on Earth surface rise up only with 10%

http://www.bas.bg/


Ulysses reveals global solar wind plasmaUlysses reveals global solar wind plasma

http://www.nasa.gov/topics/solarsystem/features/ulyssesr-20080923.html

http://www.bas.bg/


GCR spectra observed at L values greater than 5GCR spectra observed at L values greater than 5

ISS; MDU#4; July 6-13 2001; >20 g/cm ^2 Foton M2; R3D-B2; June 1-12 2005; 1.81 g/cm ^2 Foton M3; R3D-B3; Sept.14-26 2007; 0.75 g/cm^2Foton M3; Liulin-Photo; Sept 14-26 2007; >5 g/cm^2ISS; R3DE; 20 Febr.-20 March 2008; 0.4 g/cm ^2

ISS; R3DE; L>5; 360 km; 12 uGy/h; 29.4 uSv/h; 74%

Foton M3; L-Photo; L>10; 11.1 uGy/h; 29.1 uSv/h; 78%

Foton M3; R3D-B3; L>10; 10.3 uGy/h; 27.2 uSv/h; 78%

Foton M2; R3D-B2; L>10; 7.38 uGy/h; 16 uSv/h; 79 %

ISS; L>2.8, 6.41 uGy/h; 14.6 uSv/h; 71%

0.1 1.0 10.0Deposited energy (MeV)

1E-3

1E-2

1E-1

1E+0

Dep

. Do

se (

uG

y/h

)

The doses created by GCR particles The doses created by GCR particles depends by the phase of the solar cycle depends by the phase of the solar cycle and by the thickness of shielding before and by the thickness of shielding before the detector. The neutron component is the detector. The neutron component is higher than 70% and well coincide with higher than 70% and well coincide with Phantom TORSO NASA TEPC 71% and Phantom TORSO NASA TEPC 71% and

DOSTEL 78%DOSTEL 78%

http://www.bas.bg/


Sequence of Foton M3 60 seconds data with observations of Sequence of Foton M3 60 seconds data with observations of other radiation belt relativistic electrons and SAA regionother radiation belt relativistic electrons and SAA region

S N S N S N S N S N SS N S N S N S N S N S

On the energy-time 3D diagram the On the energy-time 3D diagram the relativistic (>1 MeV) electron bursts relativistic (>1 MeV) electron bursts are seen with are seen with red color barsred color bars in the in the upper panel and with black bars upper panel and with black bars

above 500 counts per minute in the above 500 counts per minute in the lower panel. In this case the R3D-B3 lower panel. In this case the R3D-B3 spectra in Northern “N” and Sothern spectra in Northern “N” and Sothern “S” hemisphere are relatively short “S” hemisphere are relatively short

and reach up to 50and reach up to 50thth channel; channel;

The 3 cases of crossing of inner The 3 cases of crossing of inner radiation belt in the region of SAA radiation belt in the region of SAA are shown with labels “SAA”. The are shown with labels “SAA”. The

spectra in SAA are much wider spectra in SAA are much wider reaching even the 256reaching even the 256thth channel. channel.

SAA SAA SAASAA SAA SAA

http://www.bas.bg/


Example of observation of relativistic electrons Example of observation of relativistic electrons with R3DE instrument on ISS on 28 February 2008 with R3DE instrument on ISS on 28 February 2008

Relativistic (>1 MeV) electron bursts Relativistic (>1 MeV) electron bursts with maximum duration few minutes with maximum duration few minutes was observed by us first at the Foton was observed by us first at the Foton

M2 satellite behind 1.75 g/cmM2 satellite behind 1.75 g/cm22 shielding. The maximmum dose shielding. The maximmum dose observed is 304 observed is 304 Gy/h at 280 km Gy/h at 280 km

altitude.altitude.

At Foton M3 satellite behind 0.71 At Foton M3 satellite behind 0.71 g/cmg/cm22 shielding the maximmum dose shielding the maximmum dose

observed is 2314 observed is 2314 Gy/h at 295 km Gy/h at 295 km altitude.altitude.

At the EuTEF platform of Columbus At the EuTEF platform of Columbus module at ISS with R3DE instrument module at ISS with R3DE instrument behind less than 0.4 behind less than 0.4 g/cmg/cm22 shielding shielding the maximmum dose is the maximmum dose is 19195 19195 Gy/hGy/h

at 361 km altitude. The flux of at 361 km altitude. The flux of electrons reach electrons reach 8363 cm8363 cm-2-2 s s-1-1..

http://www.bas.bg/


REP observed on ISS on 5th of March 2008 between 14:27REP observed on ISS on 5th of March 2008 between 14:27and 14:46 hourand 14:46 hour

http://www.bas.bg/


Geographic positions of radiation sources Geographic positions of radiation sources selecting criteriaselecting criteria

Gmag=0.21 Gauss (SAA)

Magnetic Equator

-180-150-120 -90 -60 -30 0 30 60 90 120 150 180Longitude (Deg)

-50-30-10103050

Lat

itu

de

(deg

)0.9<L<1.1

L>2.8

http://www.bas.bg/


Different radiation sources seen in Foton M3 data with lid Different radiation sources seen in Foton M3 data with lid open/closedopen/closed

The GCR dose and flux for L>10 are The GCR dose and flux for L>10 are higher (11.12 higher (11.12 Gy/h) when lid is Gy/h) when lid is

closed (11.04 closed (11.04 Gy/h), because the Gy/h), because the secondary's and neutrons produced secondary's and neutrons produced

in the shield in the shield

When the lid of Biopan 6 is When the lid of Biopan 6 is closed (~5.8 g/cmclosed (~5.8 g/cm22) only protons ) only protons from the region of SAA and GCR from the region of SAA and GCR penetrate down to the detector of penetrate down to the detector of

R3D-B3 R3D-B3

When the lid is open (0.81 g/cmWhen the lid is open (0.81 g/cm22) , ) , because of lower shielding because of lower shielding

relativistic electrons with energy relativistic electrons with energy above 1 MeV start to penetrate to above 1 MeV start to penetrate to

the detector alsothe detector also

0 3 6 9 12 15L value

Foton M3; R3D-B3Septem ber 14-26 2007

1E+0

1E+1

1E+2

1E+3

Flu

x (c

m^

-2 s

^-1

)

1E+0

1E+1

1E+2

1E+3

Do

se (

uG

y/h

)

1E+0

1E+1D

/F (

nG

y cm

^2/

even

t)

Lid open (0.81 g/cm ^2)

Lid closed (~5.8 g/cm ^2)

ORB electrons ORB electrons

SAASAA

ORBORB

GCRGCR

http://www.bas.bg/


Comparison of data obtained at Foton M3 by R3D-B3 instrument Comparison of data obtained at Foton M3 by R3D-B3 instrument outside and Liulin-Photo instrument inside the capsuleoutside and Liulin-Photo instrument inside the capsule

http://www.bas.bg/


Main characteristics of the measurements by R3DE in Main characteristics of the measurements by R3DE in geographic coordinates, in which the dose is more than 100 geographic coordinates, in which the dose is more than 100

mGy/h in period 20 February- 20 March 2008mGy/h in period 20 February- 20 March 2008

Descending data are clustered Descending data are clustered around evening UT, while ascending around evening UT, while ascending

around morning UT. around morning UT.

Very high doses (Up to 19 mGy/h) in the Very high doses (Up to 19 mGy/h) in the regions equatorialward from magnetic poles regions equatorialward from magnetic poles

are generated by relativistic (>1 MeV) are generated by relativistic (>1 MeV) electrons, which seems to be the first electrons, which seems to be the first

observation of them at ISS.observation of them at ISS.

Small difference in the averaged altitude of SAA Small difference in the averaged altitude of SAA data in descending (353 km) and ascending (351 data in descending (353 km) and ascending (351

km) orbits can’t describe the large (with km) orbits can’t describe the large (with 56 56 mGy/h) averaged descending doses.mGy/h) averaged descending doses.

Places of observations of relativistic Places of observations of relativistic electrons are separated in narrow latitudinal electrons are separated in narrow latitudinal range equatorialward from magnetic poles. range equatorialward from magnetic poles.

The calculated values of the incident proton The calculated values of the incident proton energies in SAA region fall down from about energies in SAA region fall down from about 60 MeV at the west edge of the anomaly to 10 60 MeV at the west edge of the anomaly to 10

MeV at the east edge.MeV at the east edge.

-120 -90 -60 -30 0 30 60 90 120 150 180Longitude (deg.)

100

1000

10000

Dos

e (u

Gy/

hour

)

-60-40-20

0204060

Latit

ude

(deg

.)

1

10

100

D/F

(nG

y cm

^2/p

.)R3DE; EuTEF, C olum bus; ISS 20 Febr. - 20 M arch, 2008 Dose>100 uG y/h

340

350

360

370

Alti

tude

(km

)

0.004.008.00

12.0016.0020.0024.00

UT

(ho

urs)

1

10

100

Inc.

ene

rgy

(MeV

)

DescendingAscending

http://www.bas.bg/


Geographic positions of radiation sources Geographic positions of radiation sources

-180-150-120 -90 -60 -30 0 30 60 90 120 150 180Longitude (Deg)

-50-30-10103050

Lat

itu

de

(deg

)

++ ISS, ISS, R3DER3DE; EuTEF, Feb.-Mar. 2008; D>100 ; EuTEF, Feb.-Mar. 2008; D>100 Gy/hGy/h

-180-150-120 -90 -60 -30 0 30 60 90 120 150 180Longitude (Deg)

-50-30-10103050

Lat

itu

de

(deg

)+ + Foton M3, Foton M3, R3D-B3R3D-B3; Sept. 2007; D>50 ; Sept. 2007; D>50 Gy/hGy/h

0.81 g/cm0.81 g/cm22

0.4 g/cm0.4 g/cm22

-180-150-120 -90 -60 -30 0 30 60 90 120 150 180Longitude (Deg)

-50-30-10103050

Lat

itu

de

(deg

)

1.75 g/cm1.75 g/cm22

+ + Foton M2, Foton M2, R3D-B2R3D-B2; June 2005; D>50 ; June 2005; D>50 Gy/hGy/h

http://www.bas.bg/


ISS and Foton M3 global distributions of the averaged dose in ISS and Foton M3 global distributions of the averaged dose in pixels Long=10°, Lat=5°pixels Long=10°, Lat=5°

R3DE, EuTEF, ISS global distribution of the dose data 20 February-20 March 2008

R3D-B3, Foton M3 global distribution of the dose data 14-24 September 2007

http://www.bas.bg/


Comparison of the observed doses at 3 satellitesComparison of the observed doses at 3 satellites

3.00 4.00 5.00 6.00L value

1E+0

1E+1

1E+2

1E+3

1E+4

1E+5

1E+0

1E+1

1E+2

1E+3

1E+4

1E+5

1E+0

1E+1

1E+2

1E+3

1E+4

1E+5

Dos

e (u

Gy.

h^-1

)

Foton M 2; 1-12 June 2005; 1 .85 g .cm ^-2

Foton M 3; 14-24 Sept. 2007; 0 .71 g .cm ^-2

ISS ; 20 Feb. - 20 M arch 2008; 0 .41 g.cm ^-2

High doses are regularly observed High doses are regularly observed on Foton M2/M3 satellites in the on Foton M2/M3 satellites in the

Southern hemisphere at latitudes Southern hemisphere at latitudes above the inclination oof ISS above the inclination oof ISS

ORB

-90

-70

-50

-30

-10

10

30

50

70

90

-180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180Longitude

Lat

itu

de

ORB

The REP on ISS are rare and very The REP on ISS are rare and very sporadic. Till the wholesporadic. Till the whole

operation period of the R3DE operation period of the R3DE instrument on ISS betweeninstrument on ISS between

February and July 2008 we have only February and July 2008 we have only 8 events when the8 events when the

doses are above 2000 μGy.hdoses are above 2000 μGy.h-1-1

http://www.bas.bg/


Conclusions for REPConclusions for REP

If we will consider that the danger for the astronauts being on EVA relativistic electrons events are with dose above 500 μGy.h-1 than for the period 22 February 18 March 2008 we collect totally 132 10 seconds intervals, which is only 22 minutes. From other hand this observations are made in very low solar activity. The long period observations with SAMPEX satellite and others show increase of the REP observations when the solar activity is larger. This confirm another time the necessity of permanent active monitoring of the ISS radiation environment

http://www.bas.bg/


Examples of the averaged spectra shapes and Examples of the averaged spectra shapes and slopes for almost all available data. From below slopes for almost all available data. From below to up spectra are ordered in dependence of the to up spectra are ordered in dependence of the absorbed dose. Lowest is from ground natural absorbed dose. Lowest is from ground natural

radiation = 0.12 while the highest = 9000 radiation = 0.12 while the highest = 9000 Gy/h is Gy/h is from relativistic electron measurements at ISS.from relativistic electron measurements at ISS.

Characterization by spectrumCharacterization by spectrumshape and slopeshape and slope

ISS; MDU#4; July 6-13 2001CSA aircraft; MDU#5; 5 May - 28 June 2002Foton M2; R3D-B2; June 1-12 2005CSA aircraft; MDU#5; 6 May - 25 June 2005Jungfrau; 3450 m a.s.l.; Nov.2005-Feb. 2006Foton M3; R3D-B3 & Liulin-Photo; Sept.14-26 2007HotPay-2 rocket; Liulin-R; 31 January 2008ISS; R3DE; 20 Febr.-20 March 2008Jungfrau; 3450 m a.s.l.; Nov. 2005-Feb. 2006ALOMAR, 380 m a.s.l.; Jan.-Feb. 2008

0.1 1.0 10.0Deposited energy (MeV)

1E-5

1E-4

1E-3

1E-2

1E-1

1E+0

1E+1

1E+2

1E+3

Dep

. Do

se (

uG

y/h

)

GCRGCR

ORBORB

SAASAA

ISS; R3DE; Outer RB; 8994 uGy/h; 9791 uSv/h; 10.2%

Foton M3; ORB; 1527 uGy/h; 1632 uSv/h; 7.3%

ISS; R3DE; SAA; Ch15>50; 354 km; 929 uGy/h; 1208 uSv/h

Foton M2; SAA; Ch15>30, 283 km, 220 uGy/h; 285 uSv/h

ISS; SAA; D>100, 150 uGy/h; 195 uSv/h

Foton M3; SAA; Cha 15 >30; 187 uGy/h; 242 uSv/h

Foton M3; L-Photo; SAA, Cha15>30; 152 uGy/h; 197 uSv/h

Foton M2; ORB, SH, 293 km; 128 uGy/h; 143 uSv/h; 12%

Foton M2; L>2.8; 283 km; 14.1 uGy/h; 26.3 uSv/h; 58%

ISS; SPE; L>5; D>10; 12.1 uGy/h; 15.8 uSv/h; 42% (k=1.3)

Foton M3; L-Photo; L>10; 11.1 uGy/h; 29.1 uSv/h; 78%

Foton M3; R3D-B3; L>10; 10.3 uGy/h; 27.2 uSv/h; 78%

ISS; D2; ORB; 3.5<L<5; ch1>90; 9.16 uGy/h; 16 uSv/h; 53%

HotPay-2; Liulin-R; GCR; Dose=8.9 uGy/h

ISS; L>2.8, 6.41 uGy/h; 14.6 uSv/h; 71%

CSA; 2002 & 2005; Lat.>50° Alt.>10.6 km; 1.96 uGy/h

ISS; Magn. eq.; 1.48 uGy/h; 2.58 uSv/h; 53%

Foton M2; 0.9<L<1.1; 271 km; 1.25 uGy/h; 2.78 uSv/h; 70%

CSA; 2002 & 2005; Lat.<35°; Alt.>10.6 km; 0.96 uGy/h

Jungfrau; 3450 m. a.s.l.; Nov. 2005-Feb. 2006; 0.156 uGy/h

ALOMAR; 300 m. a.s.l.; 23 Jan-24 Feb. 2008; 0.12 uGy/h

http://www.bas.bg/


1.0 10.0D eposited energy (M eV)

1E+0

1E+1

1E+2

1E+3

Cou

nts

Calibrations at UCL, Belg ium P rotons; 7.8 M eV incident energy Norm al to the detector

Characterization of the type of radiation source by the shape and Characterization of the type of radiation source by the shape and slope of the spectraslope of the spectra

1.0 10.0Deposited energy (MeV)

1E-4

1E-3

1E-2

1E-1

1E+0

1E+1

1E+2

1E+3

Dep

osi

ted

Do

se (

uG

y/h

)

R3DBE spectraEuTEF, ISS; 20 Febr.-19 March 2008

O R B; L>3.5; D =1660

O R B; L>3.5; D =257

M ean spectra o f S AA; D =255

N W est edge o f S AA ; D =110

S East edge o f SAA ; D =103

G C R &O R B; L>3.5; D =11.4

G C R ; L<1.5 ; D =1.59

Sky blue and Sky blue and light brownlight brown lines presents 2 lines presents 2 different dose level spectra of the other belt different dose level spectra of the other belt relativistic electrons, which are observed till relativistic electrons, which are observed till

2.5 MeV depsited energy. Further the 2.5 MeV depsited energy. Further the spectrum coincide with the GCR spectrum. spectrum coincide with the GCR spectrum.

BlueBlue (NW edge), (NW edge), black (black (Mean) and Mean) and redred (SE (SE edge) lines presents 3 different positions edge) lines presents 3 different positions

spectra in the region of SAA. spectra in the region of SAA.

GreenGreen (L>3.5)(L>3.5) and and magenta (1.5<L)magenta (1.5<L) lines lines presents 2 different positions GCR spectra presents 2 different positions GCR spectra

with respective doses of 11.4 and 1.59 with respective doses of 11.4 and 1.59 Gy/hGy/h

The change of slope at 6 MeV deposited The change of slope at 6 MeV deposited energy is at the place where protons with energy is at the place where protons with

energy 6 MeV are stopped in the detector energy 6 MeV are stopped in the detector

http://www.bas.bg/


Characterization of the type of incident ions Characterization of the type of incident ions by the shape of the spectra in the region of SAAby the shape of the spectra in the region of SAA

536.6536.6Protons Protons

HydrogenHydrogenIonsIons

for 10 sfor 10 s

16.6=3%16.6=3%HeliumHelium

IonsIonsfor 10 sfor 10 s

Explanation of the shape of the Explanation of the shape of the spectrum with 2 maximums created by spectrum with 2 maximums created by

protons and helium ions. About 3% of all protons and helium ions. About 3% of all counts in SAA are created by Helium ions counts in SAA are created by Helium ions and protons falling at large angle toward and protons falling at large angle toward

the detector the detector

http://www.bas.bg/


Comparison of dose asymmetries with theComparison of dose asymmetries with theglobal distribution of the upper atmosphere neutral densityglobal distribution of the upper atmosphere neutral density

-180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180

Longitude (Deg)

-50

-30

-10

10

30

50Lat

itu

de

(D

eg)

-50

-30

-10

10

30

50

Do

se (

uG

y/h

ou

r)

Ascending orbits, 05:00 UT

Descending orbits, 18:00 UT

ISS, EuTEF, R3DE, 20 Febr.-12 March 2008

0.20.81.82.73.54.5610203050100200300400500650

Ascending: MD=740; MF=133; MUT=5.86Descending: MD=1072; MF=171; MUT=20.15

http://www.bas.bg/


Geometry of the R3DE detector against the predominateGeometry of the R3DE detector against the predominateSAA proton drift from West to East SAA proton drift from West to East

http://www.bas.bg/


ConclusionsConclusions

Long term increase of the GCR flux and dose in the declining phase of the solar cycle was Long term increase of the GCR flux and dose in the declining phase of the solar cycle was experimentally observed;experimentally observed;

Relativistic electrons and doses produced by them was first observed on ISS;Relativistic electrons and doses produced by them was first observed on ISS;

The comprehensive analysis of the Liulin type instruments data and spectra gives opportunity to by The comprehensive analysis of the Liulin type instruments data and spectra gives opportunity to by characterized:characterized:

- different radiation sources in space, in atmosphere and on ground;- different radiation sources in space, in atmosphere and on ground;

- the incident energy of the incoming to the detector protons;- the incident energy of the incoming to the detector protons;

- the type of incoming to the detector ions;- the type of incoming to the detector ions;

http://www.bas.bg/


Thank youThank you

http://www.bas.bg/


Zheng, Y., A. T. Y. Lui, X. Li, and M.-C. Fok Zheng, Y., A. T. Y. Lui, X. Li, and M.-C. Fok Characteristics of 2–6 MeV Characteristics of 2–6 MeV electrons in the slot region and inner radiation beltelectrons in the slot region and inner radiation belt, J. Geophys. Res., 111, , J. Geophys. Res., 111,

A10204, doi:10.1029/2006JA011748, 2006.A10204, doi:10.1029/2006JA011748, 2006.

http://www.bas.bg/

Documents

New space and solar weather results obtained by R3DE instrument on EuTEF platform of ISS in 2008