Science outreach on NIF: possibilities for astrophysics experiments Presentation to the SABER workshop, Stanford Linear

1. Science outreach on NIF: possibilities for astrophysics experiments Presentation to the SABER workshop, Stanford Linear Accelerator Center, March 15-16, 2006 Bruce A. Remington Group Leader, HED Program Lawrence Livermore National Laboratory

2. Intro We are implementing a plan for university use of NIF fy05 fy06 fy07 fy08 fy09 fy10 fy11 fy12 Start 3 university teams Develop full-NIF univ. use proposals Add 1-2 university teams/year Select, prepare for 1st univ. use experiment • Issues: • funding for the universities • targets • coordination with the other facilities • - Omega/NLUF, Z/ZR, Jupiter, Trident, … • proposal review committee • - assess science impact, facility capability, readiness Start university experiments (goal: ~10% of NIF shots)

3. Intro Three university teams are starting to prepare for NIF shots in unique regimes of HED physics Astrophysics - hydrodynamics Nonlinear optical physics - LPI Planetary physics - EOS Chan Joshi, PI, UCLA Warren Mori, UCLA Christoph Niemann, UCLA NIF Prof. Bedros Afeyan, Polymath David Montgomery, LANL Andrew Schmitt, NRL LLNL LPI team Paul Drake, PI, U. of Mich. David Arnett, U. of Arizona, Adam Frank, U. of Rochester, Tomek Plewa, U. of Chicago, Todd Ditmire, U. Texas-Austin LLNL hydrodynamics team Raymond Jeanloz, PI, UC Berkeley Thomas Duffy, Princeton U. Russell Hemley, Carnegie Inst. Yogendra Gupta, Wash. State U. Paul Loubeyre, U. Pierre & Marie Curie, and CEA LLNL EOS team

4. Astrophysics Supernova experiments on NIF will address the core penetration discrepancy in SN1987A Jet model • Simulations do not reproduce • observed core penetration velocities Spherical shock model Shock front SN1987A 9 x 109cm Core H He Khokhlov, Ap. J. 524, L107 (1999) Kifonidis, Ap. J. Lett 531, L123 (2000) Core Density 5 x 1011cm 6 x 109cm • Does He shell breakup allow core spikes to escape? • Are differences in 3D vs 2D spike velocities important? • How do 3D perturbations on multiple interfaces interact? • How does the initial perturbation spectrum affect the late-time evolution? [Courtesy of R. Paul Drake et al.]

5. Astrophysics The SN team is designing a divergent RT experiment for NIF to address these SN issues g/cc 0.40 0.35 0.30 0.25 0.20 0.15 0.10 0.05 0.00 t = 0 ns t = 50 ns Light foam  = 0.05 g/cc Core Heavy foam  = 0.5 g/cc Laser Ti shell (core)  = 4.5 g/cc gas  = 5.0e-5 g/cc 1 mm 1 mm [Simulations by Aaron Miles (2004)] • Mass-scaled to SN with representative Core/He, He/H, and H/ISM interfaces • Designed to address issues of: multi-interface interaction, divergence, initial conditions, 3D vs 2D, turbulent vs non-turbulent instability evolution, code validation • Can be scaled up in size, energy, and complexity, as NIF evolves [Courtesy of R. Paul Drake et al.]

6. Astrophysics NIF has already demonstrated nonlinear, shock driven, 3D hydrodynamics experiments 3D perturbation 2D perturbation Triple point Mach reflection Transmitted shocks v2 v1 Hole rarefaction Shocks Aluminum Velocity discontinuity Reflected shock 2D jet @ t = 22 ns 3D jet @ t = 22 ns 200 um 200 um 200 um [Brent Blue et al., PRL 94, 095005 (2005); PoP 12, 056313(2005)]

7. Ice crystals He drop formation? Fluid H2 + He 7700 GPa 16000 K Fluid metallic H + He 200 GPa 5300 K Phase separation? Ices? Planetary phys. High pressure experiments on NIF will address key questions regarding the internal structure of Jupiter 104 Super giants Earth Jupiter ~ keV 102 Hugoniot Isentrope; planetary interiors Internal energy, E/(K0V0) 100 K0= Bulk modulus: ~ 1 Mbar at P = 0 ~ eV 3.0 2.0 1.5 Pre-compression, /0 10-2 1.1 Key Questions: • Equation of state near the planetary isentropes • Location of the insulating-conducting transition • Melt line at high pressure • Existence of a plasma phase transition (PPT) • Does He and H2 phase separate in Jupiter/Saturn ~Mbar ~Gbar 10-1 100 101 102 103 104 Pressure, P/K0 [Courtesy of Raymond Jeanloz et al.]

8. Planetary phys. Coupling NIF with DAC targets will enable key measurements of planetary interior states Shocks with precompression Ramp-wave compression on NIF sample quartz plate Omega 104 PPT (Saumon) LIL Jupiter Neptune NIF PPT (Bonev) Visar Temperature (K) 103 Melt crv High energy laser 102 0 100 200 300 Pressure (GPa) • Pre-compression is the only way to study dense He+H2 mixtures • The PPT accessed with pre-compressions > 1 GPa • Melt curve maximum accessed with pre-compressions ~ 30 GPa • Ramp wave compression may allow planetary core conditions to be accessed [Courtesy of Raymond Jeanloz et al.]

9. Planetary phys. The NIF VISAR diagnostic and pulse shape have been demonstrated for possible shock EOS experiments 0.8 Quartz Al baseplate Preheat shield 0.6 Ablator Total power (TW) 0.4 NEL pulse shape designed to produce a 23 Mbar steady shock in Cu NIF drive 0.2 NIF VISAR trace (2004) 0 0 1 2 3 4 5 Time (ns) Predicted breakout profile 10 30 Time (ns) 8 20 Shock Vel. (km/s) Shock msmt in quartz window on NEL 10 6 -400 -200 0 200 400 Position (m) 7 8 9 Time (ns) [Courtesy of Raymond Jeanloz et al.]

10. Nonlinear interactions of intense laser beams in large scale plasmas is a scientific challenge of considerable importance Nonlin. opt’l Single beam, I > Ithr, t = 312 0/cs Single beam, I > Ithr, t =  2000 2000 z/0 1000 z/0 1000 [Schmitt & Afeyan, PoP 5, 503 (1998)] 0 0 0 x/0 500 0 x/0 500 I < Ithr, sub-thresh. crossing beams can filament, due to interactions with IAW fluctuations I < Ithr, single-beam simulation, no filamentation Beam 1 Beam 1 [Courtesy of Andy Schmitt & Bedros Afeyan Beam 2 Without interacting beams • Filamentation strongly affects the initiation and evolution of • SRS and SBS backscatter, as well as beam pointing

11. driver beams driver beams probe beams Nonlin. opt’l NIF will allow experiments probing the interaction of multiple beams in large scale plasmas over a wide range of (ne,Te) • HYDRA simul’s show that high plasma • temperatures (Te = 3-6 keV) and densities • (ne =0.1 critical) can be achieved Early time: driver beams explode foil • Crossing beams will allow non-resonant effects • on SRS backscatter to be studied with good • speckle statistics • NIF’s versatile pulse-shaping will greatly expand • the design space for exploding foil targets Laser pulse shapes Late time: probe beams interact with drive beams and long, hot plasma. red =“hot case” 2  Laser intensity x 1015 (W/cm2) 1 black=“cool case” 0 0 2 4 Time (ns) [Courtesy of Chan Joshi et al.]

12. Nonlin. opt’l The FABs and NBI diagnostics have already measured angularly resolved scattered energy with high precision on NIF 1.2 kJ SBS out side lenses 153 J in lenses 130 J SRS out side lenses 38 J SRS in lenses (High temperature hohlraum target experiment) [Glenzer et al., Nucl. Fusion 44, S185 (2004)] [Courtesy of Chan Joshi et al.]

13. Summary Our vision for university use of NIF is to coordinate with the other HED facilities in a staged approach • Test out new ideas, develop new techniques, on smaller facilities, such as Janus, • Trident, Titan, Vulcan, Helen, Cornell X-pinch, Nevada Terawatt Facility, Magpie, … • Example: Collins, Jeanloz et al., laser-DAC experiments on Vulcan • Promising ideas move to major HED facilities, such as Omega, Z/ZR, Saturn, • LIL, … for demonstration on “big machines”: • Examples of Omega / NLUF: • “Optical Mixing Controlled Stimulated Scattering Instabilities,” Bedros B. Afeyan et al. • “Recreating Planetary Core Conditions on Omega,” Raymond Jeanloz et al. • “Experimental Astrophysics on the Omega Laser,” R. Paul Drake et al. • Those experiments requiring high energy “conclusion points” then propose to NIF • Informal coordination between the facilities appears possible

14. HED laboratory astrophysics allows unique, scaled testing of models of some of the most extreme conditions in the universe • Stellar evolution: opacities (eg., Fe) relevant to stellar envelopes; • Cepheid variables; sellar evolution models; OPAL opacities • Planetary interiors: EOS of relevant materials (H2, H-He, H20, Fe) • under relevant conditions; planetary structure - and • planetary formation - models sensitive to these EOS data • Core-collapse supernovae: scaled hydrodynamics demonstrated; • turbulent hydrodynamics within reach; aspects of the • “standard model” being tested • Supernova remnants: scaled tests of shock processing of the ISM; • scalable radiative shocks within reach • Protostellar jets: relevant high-M-# hydrodynamic jets; • scalable radiative jets, radiative MHD jets; • collimation quite robust in strongly cooled jets • Black hole/neutron star accretion disks: • scaled photoionized plasmas within reach • Our goal: to be citius, altius, fortius, sapientius for laboratory astrophysics • [Roger Blandford, keynote address, HEDLA-04]