Experimental Observation of a Radiative Wave Generated in Xenon by a Laser-Driven Supercritical Shock

Bozier, J. C.; Thiell, G.; Breton, J. P. Le; Azra, S.; Decroisette, M.; Schirmann, D.

doi:10.1103/physrevlett.57.1304

Cited by 86 publications

(61 citation statements)

References 12 publications

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“…Sect. 7 below for the Case of xenon initially at 1.3 × 10 −3 g/cm 3 and 300 K, using perfect-gas equation-of-state (γ = 5/3 and mean molecular weight μ = 20 equivalent to a mean ionization stage of 5), and analytic opacities (Bozier et al 1986). The shock propagates from top to bottom.…”

Section: Effect Of Radiative Lossesmentioning

confidence: 99%

“…1. These academic profiles were obtained using xenon with a constant ionisation charge of 5, a perfect-gas equation-of-state with γ = 1.1, and analytic opacities (Bozier et al 1986). The velocity of the shock is 65 km s −1 and the initial density and temperature are 1.3 × 10 −3 g/cm 3 and 300 K, respectively.…”

Section: Structure Of a 1d Radiative Shockmentioning

confidence: 99%

“…The study of radiative shocks on Earth thus require different gases and physical conditions, which can be recreated by high energy installations such as laser or pulsed electric installations (Remington et al 2006). Radiative shock experiments have been performed with high power lasers (Bozier et al 1986(Bozier et al , 2000Keiter et al 2002;Reighard et al 2006;Bouquet et al 2004;González et al 2006b;Busquet et al 2006Busquet et al , 2007. Typically, a 200 J laser in about 1 ns can launch a shock at about 60 km s −1 in targets of millimeter size (Bouquet et al 2004) filled with xenon at pressures of some fractions of bars, whereas supercritical shocks at 100 km s −1 in SiO 2 aerogel, argon, and xenon have been produced at the OMEGA laser (5 kJ).…”

Section: Introductionmentioning

confidence: 99%

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2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

González

Audit

Stehlé

2009

A&A

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Context. Radiative shocks are found in various astrophysical objects and particularly at different stages of stellar evolution. Studying radiative shocks, their topology, and thermodynamical properties is therefore a starting point to understanding their physical properties. This study has become possible with the development of large laser facilities, which has provided fresh impulse to laboratory astrophysics. Aims. We present the main characteristics of radiative shocks modeled using cylindrical simulations. We focus our discussion on the importance of multi-dimensional radiative-transfer effects on the shock topology and dynamics. Methods. We present results obtained with our code HERACLES for conditions corresponding to experiments already performed on laser installations. The multi-dimensional hydrodynamic code HERACLES is specially adapted to laboratory astrophysics experiments and to astrophysical situations where radiation and hydrodynamics are coupled. Results. The importance of the ratio of the photon mean free path to the transverse extension of the shock is emphasized. We present how it is possible to achieve the stationary limit of these shocks in the laboratory and analyze the angular distribution of the radiative flux that may emerge from the walls of the shock tube. Conclusions. Implications of these studies for stellar accretion shocks are presented.

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Section: Effect Of Radiative Lossesmentioning

confidence: 99%

Section: Structure Of a 1d Radiative Shockmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

González

Audit

Stehlé

2009

A&A

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“…This defines a threshold velocity for radiative shocks, which is for example 60 km/s in Xe at 10 mg/cm 3 and is 200 km/s in CH at 10 mg/cm 3 . The other two key dimensionless parameters are the optical depths upstream of and downstream of the shock.…”

Section: The Radiative Shock Contextmentioning

confidence: 99%

“…Laboratory studies of radiative shocks are motivated by the presence of such shocks in astrophysics [1], by the developing ability to perform radiation hydrodynamic experiments in the laboratory [2][3][4][5][6][7], and by the need for experiments to benchmark new generations of astrophysical radiation-hydrodynamic codes. In our ongoing work with collaborators [8,9] we have developed experiments that can produce these shocks and have diagnosed them by radiography and other techniques.…”

Section: Introductionmentioning

confidence: 99%

Context and Theory for Planar Radiative Shock Experiments in Xenon

Drake¹,

Reighard

2006

AIP Conference Proceedings

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Abstract. Our laboratory studies of radiative shocks include development of the semi-analytic theory that corresponds to various cases of interest to experiments, development of experiments, comparison of experiments and simulations, and drawing connections to astrophysics. Here we discuss theory and experiment of radiative shocks that are optically thin to thermal radiation in the upstream direction but optically thick in the downstream direction.

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High Energy Density Laboratory Astrophysics

Kyrala¹

2005

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Experimental Observation of a Radiative Wave Generated in Xenon by a Laser-Driven Supercritical Shock

Cited by 86 publications

References 12 publications

2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

Context and Theory for Planar Radiative Shock Experiments in Xenon

High Energy Density Laboratory Astrophysics

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