Upload
ysam2
View
28
Download
0
Embed Size (px)
Citation preview
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 1/44
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
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 2/44
MBar compressionP∆V ~ eV, Bonds change
GBar compressionP∆V ~ KeV, Atomschange
dynamic compression
2
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 3/44
NIF generates pressures found at thecenter of Jupiter
NIF will create ≥1033 neutrons per cm2 persecond, equivalent to a supernova
NIF will access unprecedented energy densities
NIF will produce enough x-ray flux tosimulate conditions in an accretion disk
NIF will create thermal plasmas at theconditions of stellar interiors
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 4/44
Hydrogen Phase space forhigh energy density science
4
L o g T e m p e r
a t u r e ( K )
Log density (g•cm-3)
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 5/44
Hydrogen Phase space forhigh energy density science
5
L o g T e m p e r
a t u r e ( K )
Log density (g•cm-3)
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 6/44
Hydrogen Phase space forhigh energy density science
6
L o g T e m p e r
a t u r e ( K )
Log density (g•cm-3)
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 7/44
Hydrogen Phase space forhigh energy density science
7
Hot spot108 K
Cold fuel1 Kg/cc
L o g T e m p e r a t u r e ( K )
Log density (g•cm-3)
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 8/44
Hydrogen Phase space forhigh energy density science
8
L o g T e m p e r a t u r e ( K )
Log density (g•cm-3)
Previousexperiments
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 9/44
Hydrogen Phase space forhigh energy density science
9
High energydensity regime toexplore with NIF
With Burning plasmas
L o g T e m p e r a t u r e ( K )
Log density (g•cm-3)
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 10/44
Time (ns)
T o t a l p o w
e r ( T W )
150
0 10 20
75
0
Withprecompressed
D-> ~5g/cc
Pulse shape ultra-high pressureplasma and solid-state experiments
Stixrude, 2008
4
2
104
8
4
2
103
8
4
0.1 1 10 100 1000
Pressure (Mbar)
T e m p e r a
t u r e ( 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 extremesolid state to fusion experiments
10
Shock
Ramp
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 11/44
Time (ns)
T o t a l p o w
e r ( T W )
150
0 10 20
75
0
WithprecompressedD-> ~5g/cc
Pulse shape ultra-high pressureplasma and solid-state experiments
Stixrude, 2008
4
2
104
8
4
2
103
8
4
0.1 1 10 100 1000
Pressure (Mbar)
T e m p e r a t u r e ( 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 extremesolid state to fusion experiments
11
Shock
Ramp
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 12/44
NIF’s high energy and pulseshaping will enableextreme solid state to fusion experiments
12
Time (ns)
T o t a l p o w
e r ( T W )
60
0 10 20
30
0
WithprecompressedD-> ~5g/cc
Pulse shape for ignition
Ignition,1019
neutronsTr ~ 5 KeV
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 13/44
VanHorn
We are just now trying to determine regimes accessiblewith ignition, this example is again for Fe
With ignition, the regimes we will be able toaccess are still more extreme
Hugoniot
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 14/44
We are just starting to develop science “platforms”to explore this new frontier of science
14
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
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 15/44
Omega experiments canaccess the few Mbar regime,~0.8 * RJupiter
NIF experiments can accessthe most extreme conditions inany 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 atMbar-Gbar conditions
NIF will be able to recreate the most extremeconditions of any planet
15
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 16/44
Russ HemleyCarnegie InstituteKev Chemistry
RaymondJeanlozU.C.Berkeley
Yogi GuptaWashington State
Solids atP>20Mbar
LLLNIF, DNT, PLS, Eng
D. StevensonCalTech
Planet Models
Lars StixrudeUniv. of MichiganExtreme Chemistry
BurkhardMilitzerEarth and
Planetary
ScienceRichard MartinU. IllinoisSolid State Theory
Justin WarkOxfordUniversity
Tom DuffyPrincetonElastic consts& rigidity
W. HubbardU. ArizonaPlanet theory
Paul LoubeyreCEAH & H/He atP>10 Mbar
Steven RoseImperial College,LondonPlasma Physics
Group
The team of leading scientists in the field ofultra-dense matter continues to grow
W. Mao (Stanford), K. Lee (Yale), R.Wentzcovitch, C. Bolme (LANL), T.Guillot, (Obs. Nice)
16
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 17/44
Many of the techniques have been benchmarked on theOmega, Jupiter, and Vulcan laser facilities
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 18/44
30 Mbar NIF design is scaled from8 Mbar Omega experiments
S t r e s s
( M b a r )
0
15
30
Density (g/cc)1062
Time (ns)
T o t a l p o w e r ( T W )100
50
00 10 20
We will discover if carbon stays solidand strong at 10’s of Mbar
Next year we will extend solid statephysics to 30 Mbars on NIF
18
Eggert, Hicks
Eggert, Braun
Metallic polymeric
fluid phase
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 19/44
Materials science/planetary interiors platform- rampcondition of Fe to super-earth conditions (~ 20 Mbar)
Target: ignition hohlraum, phaseplates; specialized drive, package Diagnostics
VISAR/SOP(90,45)
TARPOS
TAS
OPAS/
NOPAS
DANTEX-ray drive
VISAR/SOP(90,315)
D i a m o n d F e
VISAR/SOP
In addition to being able make solids at 10’s of Mbar, we can now study these solidswith diffraction, EXAFS, velocimetry, and broad band reflectance
Time (ns)
P o w e r ( T W )
100
50
0 20 40
150
0
NIF laserpulse
Advanced diagnostics are being developed to
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 20/44
Imaging 17.5 KeV image ofshocks (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 => localstructure in Fe to 3 Mbar (Hemely, Hicks)
Advanced diagnostics are being developed toexplore the microscopic physics in this densematter regime
20
Optical spectroscopy todetermine bonding (Bolme,Hemely, )
Hi-res interferometry for shock
structure (Celliers, Smith, Brygoo)
Simultaneous diffraction and velocity
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 21/44
Simultaneous diffraction and velocity
measurements give compressibility andphase to 5 Mbar
21
S t r
e s s ( M b a r )
0
1.5
3.0
Time (ns)
1050
V el o ci t y ( k m / s )
10
1.85 Mbar
3.24 Mbar
Eggert, Rygg
This is by far the highest P diffraction ever collectedand sets the stage for NIF experiments
Powder diffraction on rampcompressed samples
10 μm Fe
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 22/44
X-ray Scattering/absorption shows localstructure in Fe to 3 Mbar (Hicks)
Yacoi, Remington
Data at P = 3 Mbar
We also developed EXAFS for Ultra-hi-P solids
Determines Fe structure + coordination+T
Preliminaryanalysis suggestsHCP with c/a ~1.73
We expect thecombination of
Diff. + EXAFS willgive T
χ
Electron wavenumber (A-1)Hicks,Ping
Yakoby, Remington et al
22
Coupling diamond cells to laser shocks
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 23/44
Loubeyre 06
The technique has been demonstrated on Omega to 200 GPa, and is expected toscale to 10+ TPa on NIF (Eggert PRL 08, Jeanloz PNAS 07, Lee JCP 06, Loubeyre JHP 06)
Coupling diamond cells to laser shocksenables access to ultra-high density statesfor He, H2, He+H2
23
10 kbar
50 kbar.6 Mbar
H2
Precompressed shocks
100
1000
10000
T ( K )
Conducting fluid
Jupiter
P+e
Metal HSolid H2
Fluid H2 ~isentrope
.01 0.1 1 10 100
P(Mbar)
He
Visar
Laser
Diamond cell
Coupling diamond cells to laser shocks
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 24/44
Loubeyre 06
The technique has been demonstrated on Omega to 200 GPa, and is expected toscale to 10+ TPa on NIF (Eggert PRL 08, Jeanloz PNAS 07, Lee JCP 06, Loubeyre JHP 06)
Coupling diamond cells to laser shocksenables access to ultra-high density statesfor He, H2, He+H2
24
10 kbar
50 kbar.6 Mbar
H2
Precompressed shocks
100
1000
10000
T ( K )
Conducting fluid
Jupiter
1st NIF H2experiment
Metal HSolid H2
Fluid H2 ~isentrope
.01 0.1 1 10 100
P(Mbar)
He
Visar
Laser
Diamond cell
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 25/44
HED facilities deliver:E/V ≥ 1011 J/m3 or P ≥ 1 Mbarover spatial scales L ≥ 1 mm
Currnet ultra-dense matter plans for NIF include10’s Mbar solids & 10’s of Gbar dense plasmas
FY12FY11FY10
New regime ofSolid-state – 10
to 100’s of Mbar
Ultra-denseHydrogen
Kilovoltchem/Gigabar
press.
30 MbarCarbon6 shots
Fe-ramp to 20Mbar, 4 shots
Diffractionstructure & T4 shots
EXAFS forlocal order 4shots
50 MbarHe/H24 shots
D2 to 6 g/cc4 shots
Shock Fe to
1 Gbar4 shots Fe @ 10’s Gbar4 shots
EXAFS/diffraction at >100Mbar
4 shots
H @manyGbar
H-D 100
Mbar(Pycnonuclear)
t
Convergent experimentsAtomic scale data & H innew regime
1-D compressionIgnition hohlraumsVISAR/SOP
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 26/44
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
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 27/44
NIF will open a new field of Burning Plasmaphysics, 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
T e
,T i ( k eV )
⟩ ( g c m - 3 )
Radius (µm)
⟩
Ti
Te
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 28/44
Previous Photoionised plasmas achievedξ=20ergcms-1, NIF will achieve >1000ergcms-1
28
Low mass X-ray binaryξ=30 ergcms-1
Seyfert galaxyξ=300 ergcms-1
NIF with burning capsule
FFe
CH
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 29/44
Laboratory Astro/Nuclear Physics
29
• Measure opacities relevant to stellarevolution
- Can measure LTE and non-LTE conditionsat high T and high or low rho
• Test codes modeling turbulence on NIF
- Supernovea simulations suggest
significant mix: NIF can benchmark thesesimulations
- How were heavy elements dispersed in theUniverse
• 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 pinch1990s
Z, ZR, Omega2000-2009
NIF 2010-2015?
Kifonidis,Ap. J. Lett 531,L123 (2000)
5 x 1011cm
HFe
NIF will reach near core conditions of the sun
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 30/44
eac ea co e co d t o s o t e suand measure κRosseland to ~10%
Ti n=2 ton=1
Ti n=3to 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).)
CapsuleBacklighter
collimator
Hohlraum
X-ray flash
Hohlraumtemperature
Samplevolume with
radiography
Gated x-ray
spectrometer
Hohlraumtemperature
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 31/44
Supernovae come in two general categories
• Involve M~Msun stars• Optically brighter
• Standardized candles
• Serve as distance indicators
31
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
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 32/44
Supernovae come in two general categories
• Source of the elements up to Z ~ 26• Data behind the accelerating universe
and dark energy
32
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
T II l f h d h f
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 33/44
Type II supernovae result from the death of amassive star
33
[Hillebrandt, Sci. Am., 43 (Oct. 2006)]
Near-death, the massive star, M > 8Msun ,takes on an onion-layer structure
4 x 106 km
T II lt f th d th f
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 34/44
Type II supernovae result from the death of amassive star
34
[Hillebrandt, Sci. Am., 43 (Oct. 2006)]
Iron core collapses in ~0.1 s,at a free-fall velocity of ~c/4
T II lt f th d th f
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 35/44
Type II supernovae result from the death of amassive star
35
[Hillebrandt, Sci. Am., 43 (Oct. 2006)]
Shock
Rebound occurs whencore reaches nucleardensity, launching astrong shock
At nuclear density,ρnuclear~ 2 x 1014 g/cm3,the Earth would have aradius of only ~192 m
A “nuclear shock” is strong :
Pshock ~ 1 MeV / fm
3
~ 10
21
Mbar
200 km
ProtoneutronStar
Type II supernovae result from the death of a
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 36/44
Type II supernovae result from the death of amassive star
36
[Hillebrandt, Sci. Am., 43 (Oct. 2006)]
The shock stalls, due to the in-flowing matter, then gets revived in ~1 s byneutrino heating and the Standing Accretion Shock Instability (SASI)
Shock
ProtoneutronStar
Type II supernovae result from the death of a
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 37/44
Type II supernovae result from the death of amassive star
[Hillebrandt, Sci. Am., 43 (Oct. 2006)]
37
The shock breaks outfrom the surface of thestar in 1-2 hr, and thestar blows up as a SN
Stalled shock restarts, thenr-process nucleosynthesisoccurs for the next ~10 s
ProtoneutronStar
Type II supernovae result from the death of a
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 38/44
Type II supernovae result from the death of amassive star
38
[Hillebrandt, Sci. Am., 43 (Oct. 2006)]
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
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 39/44
P. Drake et al. are developing designs to recreatea scaled supernova explosion on NIF
39
Scaled SN1987A on NIF
Z-axis (mm)
R a d i u s ( m m )
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
0
R a d
i u 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
Drivebeams
ConcentricHemispherical
Shells
Tworippled
interfaces
HED Plasma induced excited state population is
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 40/44
HED Plasma induced excited state population isbelieved to play a role in s-process nucleosynthesis
Z
N
S-process conditions k B T ≈ 8, 30 keV ρ≈50-100 g/cm3
s-process path near Tm
169Tm 170Tm 172Tm
171Yb 172Yb 173Yb170Yb
171Tm
5.025 keV
4.8 ns3/2+
1/2+
171Tm
Dope ICF capsule with Tm, capture products from debris, measure ratioof 172/170 to determine s-process cross section enhancement factors
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 41/44
Plasma pulseamplification andcompression at NIF canproduce unprecedentedintensities on target
41
• What happens at 1025 W/cm2 ?=>photon pressure ~ 1010 Mbars
• Can we learn how cosmic
accelerators work?• Nature of laser-matterinteraction at high energy &intensity
Extreme laser intensities
J. Ren, Nature Physics, 2007
R. Kirkwood, Physics Rev. Lett., 1996
Y. Ping Submitted PRL
R. Kirkwood, Physics of Plasmas 2007
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 42/44
Plasma pulse amplification andcompression concept for NIF
42
• What happens at 1025 W/cm2 ?=>photon pressure ~ 1010 Mbars
• Can we learn how cosmic
accelerators work?• Nature of laser-matterinteraction at high energy &intensity
Extreme laser intensities
We are just starting to develop science “platforms”
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 43/44
We are just starting to develop science platformsto 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
5/13/2018 Gilbert Collins- University Use of NIF Science - slidepdf.com
http://slidepdf.com/reader/full/gilbert-collins-university-use-of-nif-science 44/44
44