Highlights_from_HEDLA_06b.ppt;1 Highlights from HEDLA-06 Presentation to the SABER workshop, Stanford Linear Accelerator Center, March 15-16, 2006 Bruce.

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Highlights_from_HEDLA_06b.ppt;1 Highlights from HEDLA-06 Presentation to the SABER workshop, Stanford Linear Accelerator Center, March 15-16, 2006 Bruce A. Remington HED Program Lawrence Livermore National Laboratory

Highlights_from_HEDLA_06b.ppt;2 High energy density (HED) implies large Energy/Volume, which is the prevailing condition in high energy astrophysics Log  (g/cm 3 ) Log T(K) Log kT(eV) Log n(H)(/m 3 ) [NRC X-Games report, R. Davidson et al. (2003)]

Highlights_from_HEDLA_06b.ppt;3 Peter Celliers: EOS of dense He showing reflectivities, 5% ionization thermally generated Ray Smith: ICE drive on laser to 2 Mbar at Omega along a quasi-isentrope Jonathan Fortney, Gilles Chabrier: planetary interior structure sensitive to EOS models, experiments Jim Hawreliak: dynamic diffraction of shocked Fe showing  transition at 120 kbar in sub-nsec Barukh Yaakobi: dynamic EXAFS of shocked Fe showing  transition at 120 kbar in sub-nsec Marcus Knudson: EOS of water, showing refreeze (Dan Dolan) Michel Koenig: absolute EOS msmt capability for Al, using K  radiography Tomek Plewa: “solved” the core-collapse SN1987A problem? Carolyn Kuranz: deep nonlinear Omega experiments relevant to SN1987A Lebedev, You, Kato: magnetic tower jets on Z-pinch, Cal Tech plasma simul. chamber, astrophys. Marc Pound: synthetic observations of Eagle Nebula models to compare with actual observations Amy Reighard:   = 50 in radiative shock in Xe gas at Omega laser Freddy Hansen: radiative shock precursor launches new shock Gianluca Gregori: XTS to get Te, Ti, ne, Z in HDM and WDM Steve Rose: photoionized plasmas (of Fe): models that put in all the levels poorly better than models that put in only some of the levels well (leaving out others). Showed Z distribution (Au, Fe) vs exp’ldata, w/, w/o rad. and/or dielectronic recomb/autoioniz Jim Bailey: exp’l opacity of Fe at conditions approaching those of the solar radiative zone Scott Wilks: PW experiments to reach high temperatures ( eV) in solid-density Cu targets Sebastien Le Pape, B = 500 MG using proton deflectometery Karl Krushelnick: B = 750 MG using high harmonics cutoffl; speculation of reconnection signature Dmitri Ryutov, John Castor, Gordienko: scaling in collisionless, intense laser experiments regime Mikhail Medvedev: Weibel instability in GRB models and in intense laser experiments Richard Klein: proposed NIF astro. exp. to achieve Te = 5 keV in (1mm) 3 solid density Anatoly Spitkovsky: pulsar winds and wind shocks Some highlights from HEDLA06

Highlights_from_HEDLA_06b.ppt;4 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 (H 2, H-He, H 2 0, 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