University Use of NIF Science · 2009-11-19 · NIF generates pressures found at the center of Jupiter. NIF will create ≥ 10. 33. neutrons per cm. 2. per second, equivalent to a

Gilbert CollinsIFSA University Use of NIFLLNL-PRES-416675

This work performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344

University Use of NIF Science

MBar compression P∆V ~ eV, Bonds change

GBar compression P∆V ~ KeV, Atoms change

dynamic compression

2

NIF generates pressures found at the center of Jupiter

NIF will create ≥1033 neutrons per cm2 per second, equivalent to a supernova

NIF will access unprecedented energy densities

NIF will produce enough x-ray flux to simulate conditions in an accretion disk

NIF will create thermal plasmas at the conditions of stellar interiors

Hydrogen Phase space for high energy density science

4

Log

Tem

pera

ture

(K)

Log density (g•cm-3)


5

Log

Tem

pera

ture

(K)



6

Log

Tem

pera

ture

(K)



7

Hot spot108 K

Cold fuel1 Kg/cc

Log

Tem

pera

ture

(K)



8

Log

Tem

pera

ture

(K)


Previous experiments


9

High energy density regime to explore with NIF

With Burning plasmasLo

g Te

mpe

ratu

re (K

)


Time (ns)

Tota

l pow

er (T

W)

150

0 10 20

75

0

With precompressedD-> ~5 g/cc

Pulse shape ultra-high pressure plasma and solid-state experiments

Stixrude, 2008

4

2

104

8

4

2

103

8

40.1 1 10 100 1000

Pressure (Mbar)

Tem

pera

ture

(K)

NIF can produce P > 1 Gbar shocks, P> 10’s Mbar for Ramp compression

Fluid

Iron

Ramp

NIF’s Pulseshaping and Burn will enable extreme solid state to fusion experiments

10

Shock

Ramp

Time (ns)

Tota

l pow

er (T

W)

150

0 10 20

75

0


Pulse shape ultra-high pressure plasma and solid-state experiments

Stixrude, 2008

4

2

104

8

4

2

103

8

40.1 1 10 100 1000

Pressure (Mbar)

Tem

pera

ture

(K)

NIF can produce P > 1 Gbar shocks, P> 10’s Mbar for Ramp compression

Fluid

Iron

Ramp

NIF’s Pulseshaping and Burn will enable extreme solid state to fusion experiments

11

Shock

Ramp

NIF’s high energy and pulseshaping will enable extreme solid state to fusion experiments

12

Time (ns)

Tota

l pow

er (T

W)

60

0 10 20

30

0


Pulse shape for ignition

Ignition, 1019

neutronsTr ~ 5 KeV

VanHorn

We are just now trying to determine regimes accessible with ignition, this example is again for Fe

With ignition, the regimes we will be able to access are still more extreme

Hugoniot

We are just starting to develop science “platforms” to explore this new frontier of science

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R. Jeanloz, T. Duffy, R. Hemley, Y. Gupta, P. Loubeyre, L. Stixrude, S. Rose, J. Wark, G. Collins

S. Rose, R. Betti, J. Meyer-Ter-Vehn, S. Atzeni, G. Collins

P. Drake, D. Arnett, A. Frank, T. Plewa, T. Ditmire, A. Takabe, B. Remington

Astro/Rad-transport & Hydrodynamics

G. Fuller, U. Greife, Z. Shayer, C. Brune, R. Boyd, L. Bernstein

N. Fisch, C. Niemann, C. Joshi W. Mori, B. Afeyan, D. Montgomery, A. Schmitt, B. Kirkwood

Omega experiments can access the few Mbar regime, ~0.8 * RJupiter

NIF experiments can access the most extreme conditions in any planet

2 Mbar

5300 K

77 Mbar

16000 K

C. J. Hamilton

Some Key Issues:• What is a solid at >10 Mbars• How does H behave at 5,10,…g/cc

• What chemistry occurs at Mbar-Gbar conditions

NIF will be able to recreate the most extreme conditions of any planet

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Russ Hemley Carnegie InstituteKev Chemistry

RaymondJeanloz U.C.Berkeley

Yogi GuptaWashington State Solids at

P>20Mbar

LLLNIF, DNT, PLS, Eng

D. StevensonCalTechPlanet Models

Lars Stixrude Univ. of MichiganExtreme Chemistry

BurkhardMilitzer Earth and

Planetary ScienceRichard Martin

U. IllinoisSolid State Theory

Justin WarkOxford University

Tom Duffy PrincetonElastic consts& rigidity

W. HubbardU. ArizonaPlanet theory

Paul Loubeyre CEA H & H/He atP>10 Mbar

Steven RoseImperial College,LondonPlasma Physics

Group

The team of leading scientists in the field of ultra-dense matter continues to grow

W. Mao (Stanford), K. Lee (Yale), R. Wentzcovitch, C. Bolme (LANL), T. Guillot, (Obs. Nice)

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Many of the techniques have been benchmarked on the Omega, Jupiter, and Vulcan laser facilities

30 Mbar NIF design is scaled from 8 Mbar Omega experiments

Stre

ss (M

bar)

0

15

30

Density (g/cc)1062

Time (ns)

Tota

l pow

er (T

W) 100

50

0 0 10 20

We will discover if carbon stays solid and strong at 10’s of Mbar

Next year we will extend solid state physics to 30 Mbars on NIF

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Eggert, Hicks

Eggert, Braun

Metallic polymeric fluid phase

Materials science/planetary interiors platform- ramp condition of Fe to super-earth conditions (~ 20 Mbar)

Target: ignition hohlraum, phase plates; specialized drive, package Diagnostics

VISAR/SOP (90,45)

TARPOS

TAS

OPAS/NOPAS

DANTEX-ray drive

VISAR/SOP(90,315)

Dia

mon

d Fe VISAR/SOP

In addition to being able make solids at 10’s of Mbar, we can now study these solids with diffraction, EXAFS, velocimetry, and broad band reflectance

Time (ns)

Pow

er (T

W)

100

50

0 20 40

150

0

NIF laserpulse

Imaging 17.5 KeV image of shocks (Hicks, Park, et al)

500 μm Qz

Omega

Shock

Diffraction for structure & strength=>Fe is HCP to 5 Mbar (Wark, Duffy, Gupta, Eggert, Harweliak, Rygg et al)

X-ray Scattering/absorption => local structure in Fe to 3 Mbar (Hemely, Hicks)

Advanced diagnostics are being developed to explore the microscopic physics in this dense matter regime

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Optical spectroscopy to determine bonding (Bolme, Hemely, )

Hi-res interferometry for shock structure (Celliers, Smith, Brygoo)

Simultaneous diffraction and velocity measurements give compressibility and phase to 5 Mbar

21

Stre

ss (M

bar)

0

1.5

3.0

Time (ns)1050

Velocity (km/s)

10

1.85 Mbar

3.24 Mbar

Eggert, Rygg

This is by far the highest P diffraction ever collected and sets the stage for NIF experiments

Powder diffraction on ramp compressed samples

10 μm Fe

X-ray Scattering/absorption shows local structure in Fe to 3 Mbar (Hicks)

Yacoi, Remington

Data at P = 3 Mbar

We also developed EXAFS for Ultra-hi-P solidsDetermines Fe structure + coordination+T

Preliminary analysis suggestsHCP with c/a ~1.73

We expect the combination of Diff. + EXAFS will give T

χ

Electron wavenumber (A-1)Hicks,Ping

Yakoby, Remington et al

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Loubeyre 06

The technique has been demonstrated on Omega to 200 GPa, and is expected to scale to 10+ TPa on NIF (Eggert PRL 08, Jeanloz PNAS 07, Lee JCP 06, Loubeyre JHP 06)

Coupling diamond cells to laser shocks enables access to ultra-high density states for He, H2, He+H2

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10 kbar

50 kbar.6 Mbar

H2

Precompressed shocks

100

1000

10000

T(K

)

Conducting fluidJupiter

P+e

Metal HSolid H2

Fluid H2 ~isentrope

.01 0.1 1 10 100P(Mbar)

He

Visar

LaserDiamond cell

Loubeyre 06

The technique has been demonstrated on Omega to 200 GPa, and is expected to scale to 10+ TPa on NIF (Eggert PRL 08, Jeanloz PNAS 07, Lee JCP 06, Loubeyre JHP 06)

Coupling diamond cells to laser shocks enables access to ultra-high density states for He, H2, He+H2

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10 kbar

50 kbar.6 Mbar

H2

Precompressed shocks

100

1000

10000

T(K

)

Conducting fluidJupiter

1st NIF H2 experiment

Metal HSolid H2

Fluid H2 ~isentrope

.01 0.1 1 10 100P(Mbar)

He

Visar

LaserDiamond cell

HED facilities deliver: E/V ≥ 1011 J/m3 or P ≥ 1 Mbar over spatial scales L ≥ 1 mm

Currnet ultra-dense matter plans for NIF include 10’s Mbar solids & 10’s of Gbar dense plasmas

FY12FY11FY10

New regime of Solid-state – 10 to 100’s of Mbar

Ultra-dense Hydrogen

Kilovolt chem/Gigabar press.

30 Mbar Carbon 6 shots

Fe-ramp to 20Mbar, 4 shots

Diffraction structure & T 4 shots

EXAFS for local order 4 shots

50 Mbar He/H2

4 shots

D2 to 6 g/cc4 shots

Shock Fe to 1 Gbar

4 shotsFe @ 10’s Gbar 4 shots

EXAFS/diffraction at >100 Mbar 4 shots

H @ many Gbar

H-D 100 Mbar (Pycnonuclear)

t

Convergent experimentsAtomic scale data & H in new regime

1-D compression Ignition hohlraumsVISAR/SOP

Burning Plasmas

• What physics limits optimizing burn?

• How does matter behave in DT burning environment, ie. Radiation and relativistic regimes?

• What are the next advanced ignition concepts?

26

NIF will open a new field of Burning Plasma physics, what are the key questions

• Understand/optimize the burning plasma

— e-ion equilibration

— Alpha deposition

— EOS/opacities and non-equilibrium

— Effects of extreme fields

— Plasma effects on nuclear reactions

• New burning plasma physics?

— Extreme neutron and photon flux

— e+e- pairs

— Photonuclear processes

27

Does a deep understanding of burning plasmas enable new ignition concepts?

Density-temperature at peak rho-R

Faster Ignition

300keV DT ions

Djaoui, JQSRT (1995), Rose

2000

1500

1000

500

00 20 40 60

10

30

50

70

Te , T

i (keV)⟩(gcm

-3)

Radius (µm)

⟩

Ti

Te

Previous Photoionised plasmas achieved ξ=20ergcms-1, NIF will achieve >1000ergcms-1

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Low mass X-ray binaryξ=30 ergcms-1

Seyfert galaxyξ=300 ergcms-1

NIF with burning capsule

FFe

CH

Laboratory Astro/Nuclear Physics

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• Measure opacities relevant to stellar evolution

- Can measure LTE and non-LTE conditions at high T and high or low rho

• Test codes modeling turbulence on NIF- Supernovea simulations suggest

significant mix: NIF can benchmark these simulations

- How were heavy elements dispersed in the Universe

• Test nuclear physics models- Benchmark excited state nuclear physics- Dense plasma effects on reaction rates- Test models for big bang nucleosynthesis- Helps to determine temperatures of stars

Saturn Z pinch 1990s

Z, ZR, Omega 2000-2009

NIF 2010-2015?

Kifonidis,Ap. J. Lett 531, L123 (2000)

5 x 1011cm

HFe

NIF will reach near core conditions of the sun and measure κRosseland to ~10%

Ti n=2 to n=1

Ti n=3 to n=1

Ti data at Omega.05 g/cc, 125 eV,

Solar Radiative Region: 200-1350 eV (Bahcall, Rev. Mod. Phys. 67, 781, 1995)

NIF 750 TW estimate from semi-emperical scaling: >700 eV(Dewald PRL 95, 215004(2005).)

Capsule Backlighter

collimator

Hohlraum

X-ray flash

Hohlraumtemperature

Sample volume with radiography

Gated x-ray spectrometer

Hohlraumtemperature

Supernovae come in two general categories

• Involve M~Msun stars• Optically brighter• Standardized candles• Serve as distance indicators

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Type II: Core CollapseType 1A: Thermonuclear

Accreting white dwarf

H He

C,OSiFe

Mantle

Envelope

Core

• Involve M >> Msun stars• More energetic• More frequent• Leaves a neutron star behind

Fe core in massive star collapses

White dwarfCompanion star

Supernovae come in two general categories

• Source of the elements up to Z ~ 26• Data behind the accelerating universe

and dark energy

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Type II: Core CollapseType 1A: Thermonuclear

Accreting white dwarf

H He

C,OSiFe

Mantle

Envelope

Core

• Source of the heavy elements, Z > 26• Questions:

− How are these elements made?− How are they ejected?

Fe core in massive star collapses

White dwarfCompanion star

Type II supernovae result from the death of a massive star

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[Hillebrandt, Sci. Am., 43 (Oct. 2006)]

Near-death, the massive star, M > 8Msun , takes on an onion-layer structure

4 x 106 km


34


Iron core collapses in ~0.1 s, at a free-fall velocity of ~c/4


35


Shock

Rebound occurs when core reaches nuclear density, launching a strong shock

At nuclear density,ρnuclear~ 2 x 1014 g/cm3,the Earth would have a radius of only ~192 m

A “nuclear shock” is strong: Pshock ~ 1 MeV / fm3 ~ 1021 Mbar

200 km

ProtoneutronStar


36


The shock stalls, due to the in-flowing matter, then gets revived in ~1 s by neutrino heating and the Standing Accretion Shock Instability (SASI)

Shock

ProtoneutronStar



37

The shock breaks out from the surface of the star in 1-2 hr, and the star blows up as a SN

Stalled shock restarts, then r-process nucleosynthesis occurs for the next ~10 s

ProtoneutronStar


38


107 km

Turbulence mixes core (blue) into the overlying He mantle (green) and H envelope (red). Some fraction of the core, carrying the synthesized heavy elements, gets ejected.

t = 5 hr

P. Drake et al. are developing designs to recreate a scaled supernova explosion on NIF

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Scaled SN1987A on NIF

Z-axis (mm)

Rad

ius

(mm

)

Ti core

0.5 g/ccCRF

0.05 g/ccCRF

0 7

7

Z-axis (mm)

5

0

t = 200 ns(1500 s in SN)

0.4 0.08 0.02

0R

adiu

s (m

m)

6

Density (g/cm3)

• Simulations show deep nonlinear mixing relevant to SN1987A• Rho-t scaling described in Ryutov et al., Ap.J. 518, 821 (1999); Ap.J. Suppl.

127, 465 (2000); Phys. Plasmas 8, 1804 (2001)]• fully developed turbulence will be experimentally studied at NIF

Simulation of Proposed Experiment

Drive beams

Concentric Hemispherical

Shells

Two rippled

interfaces

HED Plasma induced excited state population is believed to play a role in s-process nucleosynthesis

Z

N

S-process conditionskBT≈8, 30 keVρ≈50-100 g/cm3

s-process path near Tm

169Tm 170Tm 172Tm

171Yb 172Yb 173Yb170Yb

171Tm

5.025 keV4.8 ns

3/2+

1/2+

171Tm

Dope ICF capsule with Tm, capture products from debris, measure ratio of 172/170 to determine s-process cross section enhancement factors

Plasma pulse amplification and compression at NIF can produce unprecedented intensities on target

41

• What happens at 1025 W/cm2 ? =>photon pressure ~ 1010 Mbars

• Can we learn how cosmic accelerators work?

• Nature of laser-matter interaction at high energy & intensity

Extreme laser intensities

J. Ren, Nature Physics, 2007R. Kirkwood, Physics Rev. Lett., 1996Y. Ping Submitted PRL

R. Kirkwood, Physics of Plasmas 2007

Plasma pulse amplification and compression concept for NIF

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• What happens at 1025 W/cm2 ? =>photon pressure ~ 1010 Mbars

• Can we learn how cosmic accelerators work?

• Nature of laser-matter interaction at high energy & intensity

Extreme laser intensities

We are just starting to develop science “platforms” to explore this new frontier of science

43

R. Jeanloz, T. Duffy, R. Hemley, Y. Gupta, P. Loubeyre, L. Stixrude, S. Rose, J. Wark, G. Collins

S. Rose, R. Betti, J. Meyer-Ter-Vehn, S. Atzeni, G. Collins

P. Drake, D. Arnett, A. Frank, T. Plewa, T. Ditmire, A. Takabe, B. Remington

Astro/Rad-transport & Hydrodynamics

G. Fuller, U. Greife, Z. Shayer, C. Brune, R. Boyd, L. Bernstein

N. Fisch, C. Niemann, C. Joshi W. Mori, B. Afeyan, D. Montgomery, A. Schmitt, B. Kirkwood

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Documents

University Use of NIF Science · 2009-11-19 · NIF generates pressures found at the center of Jupiter. NIF will create ≥ 10. 33. neutrons per cm. 2. per second, equivalent to a