LLNL-PRES-733849

This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. Lawrence Livermore National Security, LLC

ThePursuitofIndirectDriveIgnitionattheNationalIgnitionFacilityWorkshoponPlasmaAstrophysics:FromtheLaboratorytotheNon-ThermalUniverse

Oxford,EnglandRichardTown

DeputyICFProgramLeader

July3-5,2017

LLNL-PRES-733849

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Centralhotspotinertialconfinementfusion

HotDT

ColddenseDT

MassiveimplodingshellheatscentralhotspotbyPdV

v

PPdV ~ Pr v / R

Heating

LLNL-PRES-733849

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Centralhotspotinertialconfinementfusion

HotDT

ColddenseDT

v

PPdV ~ Pr v / R

Heating

a

PFus ~ n2 T4

rRHS

=> D+T→ n 14.1MeV( )+ 4He 3.5MeV( )

4HedepositenergyinhotspotifrRHS >0.2g/cm2

*rR =Arealdensity

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Centralhotspotinertialconfinementfusion

HotDT

ColddenseDT

v

PPdV ~ Pr v / R

Heating

a

PFus ~ n2 T4

rRHS

*rR =Arealdensity

Cooling> => Ignition

PRad~ n2 T 1/2

Pe~ T 7/2 / R2

e-“Ideal”ignitionT~4keV(Fusionpower>radpower)

InpracticeneedhigherT

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Oncethehotspotignites,aburnwaverapidlyheatstherestofthefueltofusiontemperature

fburnup ≈ρR

ρR+ 6 (g/cm2 )

for total rR ~ 2 g/cm2

fburnup ≈ 25%

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IfthefueligniteswellontheNIF….

a

ColdDTshell~1000g/cm3

Pressure~350GbarrR ~1.5g/cm2

50milliondegrees~100g/cm3

~0.1mm

Energyreleased~20MJ

~1Kgofcoal

Howdowecreatesuchconditions?

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TheUnitedStatesnationalinertialconfinementfusion(ICF)programispursuing3approaches

LaserDirectDriveUniv.Rochester(OMEGA,NIF)

MagneticDirectDriveSandiaNat’lLabZ-machine

SphericalonOmega

LaserIndirectDriveLLNLNIF

Magnetizesfuel/burnproducts

Moststable InstabilitylimitsConvergence

InstabilitylimitsConvergenceandvelocity

Bettercoupling Technologyefficient,scalable

LLNL-PRES-733849

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TodaywewilltalkaboutlaserindirectdriveontheNIF

LaserDirectDriveUniv.Rochester(OMEGA,NIF)

MagneticDirectDriveSandiaNat’lLabZ-machine

Spherical on Omega

LaserIndirectDriveLLNLNIF

Moststable

LLNL-PRES-733849

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LLNL-PRES-733849

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LLNL-PRES-733849

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400MJ:storedenergyincapacitorbanks

2MJ:laserlight

10MJ:Storedinamplifiers

LLNL-PRES-733849

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OFFICIAL USE ONLY

Atherton/Hsing - JNSAC, 12

2013-

15kJ:fuel

2MJ:laserlight150kJ:capsule

LLNL-PRES-733849

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Specialshroudskeepthetargetat– 290degrees

LLNL-PRES-733849

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1 cm

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X-raypictureofcapsuletakendownaxisofthehohlraumjustbeforeashot

2mm diameter capsule

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PlasticIgnitionCapsule

~2mmdiameter

195 µm

LLNL-PRES-733849

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Thechallenge— nearsphericalimplosionby~35X

195 µm

DTshotN120716BangTime

(lessthandiameterofhumanhair)

~2mmdiameter

LLNL-PRES-733849

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Aftertheshot

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Majorchallenge:drivesymmetryatvelocityandconvergenceneededforignition– notyetpredictive

Early foot End of foot Start of main End of main

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Thecapsulemustbedesignedanddriventowithstandhydroinstabilities– reasonablypredictive

LLNL-PRES-733849

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Thecapsulemustbedesignedanddriventowithstandhydroinstabilities– reasonablypredictive

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Thecapsulemustbedesignedanddriventowithstandhydroinstabilities– reasonablypredictive

LLNL-PRES-733849

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Thecapsulemustbedesignedanddriventowithstandhydroinstabilities– reasonablypredictive

LLNL-PRES-733849

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Achievingignitionconditionsrequiresunderstandingandcontrollingtheimplosionproperties

Velocity

Shape

Entropy

MixM S

Vα

DTHotspot

DTIce

Ablator

HS

Hote- PdV worktoheathotspot

HighcompressionforrR – trapalphas,andconfinement

Conductiveandradiativecooling

EfficientconversionofimplosionKEtohotspotthermalenergy

€

RHS

€

ΔR

rRDT ~1.45g/cm2 VDT ~370km/s

RMShotspotshape<10%

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ThistalkdescribesthemainscientificresultsfromexperimentsonNIF

2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020

NationalIgnitionCampaign

HighFootcampaign

“Safe”hohlraums

1Dimplosion

Advancedhohlraums

Engineeringfeatures

Establishthecapabilitytodocontrolledimplosions

Exploremorestableimplosions

LowerLPIMoresphericalimplosions

Alternateablators

Couplingmoreenergy

Scalingstudies

LLNL-PRES-733849

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Velocity

Shape

Entropy

MixM S

Vα

DTHotspot

DTIce

Ablator

HS

Hote-

€

RHS

€

ΔR

Thenationalignitioncampaigndevelopedplatformstomeasureimplosionsandtunetheimplosion

Ge Spectra,Continuumemission

X-rayBacklitImaging

X-ray or

neutron

core image

VISARinterferometry

“Keyhole” “ConvergentAblator/ConA”

“Symcap”“DT”

X-rayPower

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Mostrequirementsweremetindividually

Velocity

Shape

Entropy

MixM S

Vα

DTHotspot

DTIce

Ablator

HS

Hote-

€

RHS

€

ΔR

rRDT ~1.45g/cm2 VDT ~370km/s

RMShotspotshape<10%

RMShotspotshape<10%

rR ~1.2-1.3g/cm2Vfuel ~350-370km/s

Butvariable

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NICimplosionsreachedignition-relevantρR≈1.3g/cm2,butneutronyieldswere<1015

130501

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0

110904

110908 110914111112

111215

120131120205

120417120920

130501

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0HF T−1HF T−1.5LFHDC VACHDC GAS

Aslaserenergywasaddedtoincreasevelocity,performancedegraded

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NICimplosionsreachedignition-relevantρR≈1.3g/cm2,butneutronyieldswere<1015

130501

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0

110904

110908 110914111112

111215

120131120205

120417120920

130501

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0HF T−1HF T−1.5LFHDC VACHDC GAS

also shown. For this implosion, the symmetric, unperturbedyield is simulated to be 3.3! 1016. Including the 2D hohl-raum asymmetries only results in a "8! reduction in yieldto 3.9! 1015. The tent perturbation alone results in a 15!yield reduction to 2.2! 1015. Surface roughness alone (notshown) results in a 5! reduction in yield. As can be seenfrom the insets, while the flux asymmetries strongly distortthe hot spot into a highly prolate shape, they do not result incold material deeply penetrating the hot spot. The tent per-turbation on the other hand injects fingers of cold DT deepinto the hot spot resulting in nearly twice the yield degrada-tion. Based on these results, the tent was evidently the domi-nant perturbation for N120321. All 2D perturbations incombination result in a 30! yield degradation to 1.1! 1015,and finally the 3D simulation results in a 50! yield

degradation to 6.0! 1014. This is close to but still slightlyhigher than the experimental yield of 4.2! 1014. Note thatthere is almost a factor of two degradation in yield between2D and 3D simulations for this highly perturbed implosion.

Fig. 4 shows the analogous implosion sequence as Fig. 2but for the higher power low foot shot N120405. The charac-teristics of the implosion sequence for N120405 are broadlysimilar to those of N120321. With the increased accelerationand convergence of this higher power implosion, however,the growth of perturbations at the ablation front is magnified.The defect caused by the tent perturbation has grown evenlarger than in N120321 and the random surface defects havegrown into larger radiating spikes. In this case, the tentdefect cuts cleanly through the north and south poles of theimploding shell roughly 150 ps before bang time and not

FIG. 2. Stagnation sequence from the 3D simulation of N120321 showing times from just before peak implosion velocity (410 ps before bang time) to the endof the simulation (160 ps after bang time). In each rendering, the outer surface shows the ablation front as defined by 1/e! the maximum density at that timeand is colored by the electron temperature with the color scale on the lower left. The left half of each cutaway shows the ion temperature with the color scaleon the upper left, and the right half of each cutaway shows the density with the color scale on the right. The temperature color scales are fixed in time, but thedensity color scale and the spatial scale change to follow the implosion in time. The dominating effect of the tent is evident at each time.

056302-5 Clark et al. Phys. Plasmas 23, 056302 (2016)

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Hydrodynamicinstabilitiesturnedouttobethebiggestproblem

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Amorestable“highfoot”laserpulsewasdeveloped

§ ReducedgrowthoftheRayleighTaylorinstabilityattheablationfront

§ Reducedimplosionconvergenceratio

1

2

46

10

2

46

100

2

4

Lase

r pow

er (

TW)

20151050Time (ns)

N120321_request N130812

N120321 low-foot N130812 high-foot

LaserpulsesforNIC(low-foot)andhigh-footdesigns

CR =Rablator,outerRhot−spot

Thehigh-footdesigntradesbetterstabilityforlowerρR andultimatefusiongain

LLNL-PRES-733849

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ExperimentalmeasurementsofRayleighTaylorgrowthconfirmedthestabilityofthehigh-foot

Lo-Footvs Hi-FootGrowthfactorat650µm

-200

0

200

400

600

800

1000

1200

0 40 80 120 160 200

Opt

ical

Dep

th G

row

th F

acto

r

Mode Number

Simulation

Low foot

Ripple target

X-ray snapshots

High

foot

RadiationhydrodynamiccalculationsofRTgrowthfactorsareveryclosetodata:PredictivecapabilityforgrowthisOK:problemistheRTgrowthseed

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Incontrastwiththelow-footNICdesign,thehigh-footyieldincreasedathighervelocity

130501

130710

130812

130927

131119

140120140304

140511

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0

0 5 10 15 200

100

200

300

400

500

Time (ns)

Lase

r Pow

er (T

W)

DU

Equator Pole

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Byusingthinnerablatorsthedesigncouldbepushedtohighvelocitiesandstagnationpressures

130501

130710

130812

130927

131119

131219

140120

140225

140304

140311

140511

140520

140707

141106

150121

150211

150401

150409

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0HF T−1HF T−1.5

130501130710

130812

130927

131119131219

140120

140225

140304

140311

140511

140520

140707

141106

150121

150211

150401150409

Coast time (ns)

Pres

sure

(Gba

r)

0 0.5 1 1.5 2 2.5 0

50

100

150

200

250

300HF T0HF T−1HF T−1.5

LLNL-PRES-733849

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Whenthevelocityofthinnershellswasincreased,theyielddropped—a“cliff”

130501

130710

130812

130927

131119

131219

140120

140225

140304

140311

140511

140520

140707

140819

141106

150121

150211

150401

150409

Laser Energy (MJ)

Neu

tron

Yie

ld

1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2.0

1015

1016HF T0HF T−1HF T−1.5

130501130710

130812

130927

131119131219

140120

140225

140304

140311

140511

140520

140707140819

141106

150121

150211

150401150409

Coast time (ns)

Pres

sure

(Gba

r)

0 0.5 1 1.5 2 2.5 0

50

100

150

200

250

300HF T0HF T−1HF T−1.5

LLNL-PRES-733849

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Asvelocityincreased,yielddroppedrelativeto1Dpredictions;2Dpredictionswerecloser

100% 35%

10%

1%

Simulated Yield

Expe

rimen

tal Y

ield

1015 1016 1017 1018

1015

1016

1D Sim2D Sim

300 km/s

340 km/s

375 km/s

spot temperature is reached despite the similar level of shellperturbations and is indicative of the tradeoff made in thehigh foot implosion. That is, by sacrificing fuel adiabat andcompressibility, the high foot implosion does not reach theperturbation levels of the low foot until much higher veloc-ities (319 compared to 390 km/s). In this case, the higher ve-locity of the high foot implosion outweighs the highercompression of the low foot such that the high foot achievessignificantly higher yield.

The likely explanation for why N140819 experienced adegradation in performance relative to other high foot implo-sions thus appears to be the reemergence of large ablationfront perturbations at higher velocities, again primarily dueto the tent. The melt feature may also have contributed,although 2D simulations suggest this was at worst a second-ary effect. In a more general sense, this high power, thinshell high foot implosion brought the high foot platform fullcircle. After reducing the ablation front perturbations to amuch tamer level with its strong first shock, as seen withN130927, N140819 was accelerated sufficiently strongly thatit returned to the perturbation levels of N120321 and began

to experience a similar degradation in yield. Recalling thatN120405, the higher power companion to N120321, mixedheavily, N140819 may indeed have been on the edge of avery steep performance cliff.

IV. HIGHER RESOLUTION 2D SIMULATIONS

It was noted in Sec. I that 2D hohlraum simulations ofthe high foot implosion series consistently over-predicted theDSR measurements for these shots. A similar over-predictionof the DSR can be seen in the 2D simulation results listed inTable III. Given this consistent over-prediction, it has beenspeculated that additional effects are present in high footimplosions, beyond those included in 2D simulations of thetype summarized in Tables II and III. In particular, it has beenhypothesized that significant supra-thermal electron pre-heat-ing50 could be occurred raising the DT fuel adiabat and reduc-ing its compressibility. Another hypothesis is that the stronglydriven high foot implosions are impacted by significant mix-ing at the fuel-ablator interface that could also heat the DTfuel and reduce its compressibility. This scenario seems

TABLE III. Summary of high foot simulation results.

N130927 N140819

2D 3D Expt. 2D 3D Expt.

Hot spot mix (ng) 0a 0a 0–150 0a 0a 0–150

Bang time (ns) 16.56 16.53 16.59 6 0.03 15.21 15.16 15.14 6 0.03

Burn width (ps) 120 143.5 188 6 30 100 110 147 6 30

X-ray P0 (lm) 31.2 31.4 35.3 6 3.0 30.9 30.5 31.3 6 2.2

X-ray M0 (lm) 39.8 45.7 49.8 6 1.5 29.5 28.8 29.9 6 1.0

PNI P0 (lm) 33.7 27.7b 32 6 4 35.6 25.3b 33.4 6 3

DSNI P0 (lm) 53.6 51.1b 55 6 4 54.7 33.3b 46.7 6 6

Tion (keV) 4.1 3.9b 4.43 6 0.15 4.5 4.4b 5.5 6 0.2

DSR (%) 4.7 3.5b 3.48 6 0.17 4.4 3.9b 3.5 6 0.2

Y13–15 MeV 6.3 ! 1015 3.1 ! 1015 4.5 6 0.1 ! 1015 1.3 ! 1016 4.3 ! 1015 5.5 6 0.1 ! 1015

aPre-loaded in DT gas.bFrom single-time post-processing at bang time.

FIG. 9. Comparison of bang time ren-derings of the high foot shot N140819and the low foot shot N120321. Bothsimulations are shown on the samecolor scales. The N140819 simulationreaches a much lower shell densitycompared to N120321 but also a muchhigher hot spot temperature accountingfor its much higher yield. It is notewor-thy, however, that despite its higheradiabat, N140819 has reached a similarlevel of shell distortion at bang timecompared to N120321. The signifi-cantly higher velocity of N140819apparently compensates for the highlevel of shell distortion and still ena-bles this implosion to achieve signifi-cant yield. Nevertheless, like the lowfoot N120321, N140819 appears to beon the edge of a cliff in performance.

056302-13 Clark et al. Phys. Plasmas 23, 056302 (2016)

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Fasterhigh-footimplosionswiththinnershellshavesimilardistortionstoNICimplosions

LLNL-PRES-733849

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Processedin-flight

radiograph

SimulatedDTfuelatstagnation

TentTent Tent

Weknowoftwomajorissues…

…andthesemaybemaskingotherfactors – e.g hydroinstability

Asymmetricx-raydrive

+

Butthereareimportantknowledgegaps(e.g.cannotseetheshell)andthemodelisnotperfect

capsule

tent

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Thetentalternativeprojectconsideredawiderangeofpossibleoptions

Tetra-cage

wires perp

to page

wires parallel

to page

low-density

(3 mg/cc)

foam

Block foam support

low-density

(~30 mg/cc)

foam

Foam shell support

Cantilevered fill-tube

supported

by additional

component

fill-tube is

cantilevered

Fishing poleFill-tube only

Fill-tube is

larger diameter

thin HDC

disk

to ensure

tangential

contact

Polar contact with diskor C re-inforced PI tent

requires 4-part

hohlraum

Near-tangential tent, standard formvar

Eliminated

MItigated

supported

by additional

component

LLNL-PRES-733849

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Includinglevitation(magnetic)butnotasaneartermproject!

NotecapsulePush-Pull

-I

+I

+I

-I +I-I

LLNL-PRES-733849

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-0.1

+0.1

-0.2

0.0

+0.2

Amplitude Δ(OD)

658 μm600 μm

30 μmfill tube

10 μmfill tube

10 μmfill tube

30 μmfill tube

300 μm offset

200 μm offset

600 μm

WehavetestedmanyconceptstomeasurethegrowthusingtheHGRplatform

30-μmthickfilltube Cantileveredfilltube SiO2 foam-shell

30 nm tent

LLNL-PRES-733849

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Wehavebeeneliminatingsupportoptionsandwilltestremainderinlayeredimplosionsthisyear

Tetra-cage

wires perp

to page

wires parallel

to page

low-density

(3 mg/cc)

foam

Block foam support

low-density

(~30 mg/cc)

foam

Foam shell support

Cantilevered fill-tube

supported

by additional

component

fill-tube is

cantilevered

Fishing poleFill-tube only

Fill-tube is

larger diameter

thin HDC

disk

to ensure

tangential

contact

Polar contact with diskor C re-inforced PI tent

requires 4-part

hohlraum

Near-tangential tent, standard formvar

Eliminated

MItigated

supported

by additional

component

✗ ✗ ✗

✗

✗

LLNL-PRES-733849

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Thehohlraum challenge:NIFscaleICFhohlraums fallroughlyintotwocategories– differentchallenges

Innerbeam

Highgasfill– LPIdominated Lowgasfill– radhydrodominated

CBET

SRS

2wp

Lowefficiency,strongtimedependentdrive

asymmetry

LLNL-PRES-733849

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Thehohlraum challenge:NIFscaleICFhohlraums fallroughlyintotwocategories– differentchallenges

Innerbeam

Highgasfill– LPIdominated Lowgasfill– radhydrodominated

CBET

SRS

2wp

Lowefficiency,strongtimedependentdrive

asymmetry

MoreefficientBettersymmetry,more

predictable?

“eliminate”LPI

Growingevidencelowgas-fillhohlraums behavemorelikesimulations

LLNL-PRES-733849

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Te - growingevidencelowfillhohlraums behavemorelikesimulationsthanLPIdominatedhohlraums

MnLyαMnHeα(y+w)MnLyα

MnHeα(y+w)

5 6 7 80

1

2

3

4

5

6

Time (ns)

Te(keV

)

MeasuredandsimulatedTe

PulseShape

2-shkHDCHegasfill,0.6mg/cc

▲▲▲▲▲▲▲▲

▲▲▲▲ ▲▲▲▲

●●

●●

●●

●●

●

▲▲▲▲

▲▲▲▲▲▲▲▲ ▲▲▲▲

△△△△△△△△

△△△△ △△△△

○○

○○

○○

○○

○

△△△△△△△△

△△△△ △△△△

3 4 5 6 7

1500

2000

2500

3000

3500

Time (ns)

DotZPosition(μm)

0.6 mg/cc, 2-shock HDCDotTrajectory

Measurement

Simulation

Simulatied Te atmeasuredtrajectory

MnLya/MnHea

OnlyafewmeasurementstodateNotyetpredictive

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Physicsoftheinnerbeamsiscomplicated– makescontrollingandpredictingsymmetrychallenging

§ Complicatedbeampath,timedependent– energydepositiondistributedinspace

§ HighZbubbleeventually“shutsoff”innerbeams–lossofcontrol

§ Ultimatelyneedthe“right”x-rayproductionoverthewaist,alsocomplicated

Motivateslargerhohlraums andshorterpulses

Mix(hydro,kinetics)

Innerbeam

e-trans

e-trans

NLTEe-trans

NLTE

Gold/HighZbubble dB/dt

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Wehavedevelopednewexperimentstoquantifyhowwelltheinnerbeammakesittothewaist

Inner-cone only

4.8 ns 5.2 ns 5.5 ns 6.2 ns

Losingsymmetrycontrol,

predictability

Innerbeams

Symmetrycontrol,predictable*

“Thin-walled”hohlraum

Combinedwithexistingsymmetrymeasurements

LLNL-PRES-733849

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Betterforlaser

Biggerhohlraumsmakethingssimpler(andeasier?)– butpracticallimit

Betterforsymmetry

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HDC’shighdensity(3.5g/cm3 comparedto1g/cm3 forCH)resultsinshorterlaserpulsesthatareeasiertofitintothehohlraum

1

2

4

68

10

2

4

68

100

2

4

Lase

r pow

er (

TW)

20151050Time (ns)

N141019_req N120321_request N130812

N120321 low-foot N130812 high-foot N141019 3-step HDC

! 27!

!!!!Figure!3! !

(d)$Si$Doped$$CH$Rev$5$$SYMCAP$

CH#1#g/cc##195um#thick##2%#Si##doped#layer##CH#1#g/cc#20#µm#thick#payload##(equivalent#mass#to#DT#ice#layer)#

1108µm#

outer#radius#1086#or#1076#µm#

HDC#ablator#86#or#76#µm#thick#3.32#g/cc#

DD##or#DT#gas#3.2#or#7#mg/cc#

DT#gas#7#mg/cc#

(a)$Un7doped$HDC$capsule$for$2$and$4$shock$$DD$or$DT$$gas$filled$Symcaps$/$1DCONA$

Outer#radius#=#1086#µm#

HDC#3.32#g/cc#86#µm#thick##THD#0.255#g/cc#58#µm#thick#

(c)$Un7doped$HDC$$with$THD$ice$layer$

T#(75%):H(23%):D(2%)#

(b)$1mm$radius$HDC$capsules$

LLNL-PRES-733849

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110608

110615 110620

110826

110904

110908 110914

111103

111112

111215

120126

120131120205

120213

120219

120311

120316

120321

120405120412

120417

120422

120626

120716

120720

120802

120808

120920

130331

130501

130530

130710

130802

130812

130927131119

131219

140120

140225

140304

140311

140511

140520

140707

140819141008

141016141106

150121

150211

150218150318

150401

150409150528

150610

160509

160807

160829

151102

160120160223

160313160418

161023

161113

170226

170601

Laser Energy (MJ)

Neu

tron

Yie

ld

0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.01014

1015

1016

CH LFCH HFHDC SC

Improveddrivesymmetry->moreefficientimplosions->higheryieldwithlessenergy

HDC2017

Highfoot2015

NIC2012

• Keywas“eliminating”LPI

• Roundimplosions

• Betteragreementwithcode

• YOC1D~30-40%

LLNL-PRES-733849

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110608

110615 110620

110826

110904

110908 110914

111103

111112

111215

120126

120131120205

120213

120219

120311

120316

120321

120405120412

120417

120422

120626

120716

120720

120802

120808

120920

130331

130501

130530

130710

130802

130812

130927131119

131219

140120

140225

140304

140311

140511

140520

140707

140819141008

141016141106

150121

150211

150218150318

150401

150409150528

150610

160509

160807

160829

151102

160120160223

160313160418

161023

161113

170226

170601

Laser Energy (MJ)

Neu

tron

Yie

ld

0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.01014

1015

1016

CH LFCH HFHDC SC

Byscaling-uptheHDCdesignwerecentlyincreasedtheyieldabove1016 forthefirsttime

HDC2017

Highfoot2015

NIC2012

N170226

N170601

c (Energy for ignition ~ 1/c 2)

Ignition(withG>1atNIF)

Alpha-heatingQa~1burningplasma(~50kJ)

Qa~2-3alphadominated(~120kJ)

(March2011)

(NIC,2012)

(highfoot,2014/15)

(HDC,2017)

LLNL-PRES-733849

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Thebestwe’vedoneonasingleshotisabout~2Xfromignition

a

ColdDTshell~1000g/cm3

Pressure~350GbarrR ~1.5g/cm2

50milliondegrees~100g/cm3

~0.1mm

Energyreleased~47kJ

~2gofcoal

~ 0.8 g/cm 2

~ 500 g/cc

~ 5 keV

~ 40 g/cc

~ 200 Gbar

Bestperformanceonsingleshot

LLNL-PRES-733849

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2020deliverableifignitionnotachieved– quantitative scalingandUQfromhighestperformancereasonablyachievable

1.8 MJ Laser Energy

Neu

tron

Yie

ld

1 MJ

100 kJ

10 kJ

1015

1016

1017

Data(highfoot,Increasingvelocity)

Quality(faster,denser,rounder,cleaner)

Energy(Bigger)

2020goal:

1. IsignitionpossibleontheNIF– “quality”?Havetomeasureandunderstandlimiters

2. Ifnot,howmuchmoreenergy isneeded?Validatedpredictivecapability+UQ

LLNL-PRES-733849

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M.J.Edwards,O.A.Hurricane,W.W.Hsing,P.K.Patel,L.F.Berzak Hopkins,M.A.Barrios,L.Benedetti,D.K.Bradley,D.A.Callahan,D.T.Casey,P.M.Celliers,C.J.Cerjan,D.S.Clark,E.L.Dewald,L.Divol,T.Döppner,J.E.Field,G.P.Grim,S.W.Haan,G.N.Hall,B.A.Hammel,M.Hermann,D.E.Hinkel,D.D.Ho,M.Hohenberger,N.Izumi,O.S.Jones,R.L.Kauffman,S.F.Khan,A.L.Kritcher,O.L.Landen,S.LePape,T.Ma,A.J.MacKinnon,A.G.MacPhee,M.M.Marinak,L.Masse,P.Michel,N.B.Meezan,J.L.Milovich,J.D.Moody,A.Moore,D.H.Munro,A.Nikroo,A.Pak,H.S.Park,J.L.Peterson,H.R.Robey,M.D.Rosen,J.S.Ross,J.D.Salmonson,M.B.Schneider,V.A.Smalyuk,B.K.Spears,P.T.Springer,M.Stadermann,D.J.Strozzi,C.A.Thomas,R.Tommasini,B.VanWonterghem,C.R.Weber

LawrenceLivermoreNationalLaboratory,Livermore,California94551,USA�

J.L.Kline,andS.Batha

LosAlamosNationalLaboratory,LosAlamos,NewMexico87545,USA�

Collaborators

LLNL-PRES-733849

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