A laser experiment for studying radiative shocks in astrophysics

Fleury, Xavier; Bouquet, S.; Stehlé, C.; Kœnig, M.; Batani, D.; Benuzzi‐Mounaix, A.; Chièze, J. P.; Grandjouan, N.; Grenier, Jason R.; Hall, Tom; Henry, E.; Lafon, J. P. J.; Leygnac, S.; Malka, Victor; Marchet, B.; Merdji, H.; Michaut, C.; Thais, F.

doi:10.1017/s0263034602202165

Cited by 51 publications

(45 citation statements)

References 8 publications

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“…The motivation behind our experiments (and behind many other experiments in laboratories around the world [8][9][10][11][12][13][14][15]) is an interest in astrophysical shocks which have high Mach numbers and which may be radiative [16], e.g., shocks originating in supernova (sn) explosions [9,[17][18][19][20]. The nature of these shocks is important to understand as the shocks mix up interstellar matter and thus a¤ect mass-loading, stellar formation [21][22][23], and the history of the Milky Way and other galaxies.…”

Section: Introductionmentioning

confidence: 99%

Secondary shock formation in xenon-nitrogen mixtures

et al. 2006

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The expansion of shock waves have been studied in mediums with di¤erent opacities and heat capacities, varied in systematic ways by mixing xenon with nitrogen keeping the mass density constant. An initial shock is generated through the brief (5 ns) deposition of laser energy (5 J) on the tip of a pin surrounded by the xenon-nitrogen mixture. The initial shock is spherical, radiative, with a high Mach number, and it sends a supersonic radiatively driven heat wave far ahead of itself.The heat wave rapidly slows to a transonic regime and when its Mach number drops to 2 with respect to the downstream plasma, the heat wave becomes of the ablative type, driving a second shock ahead of itself to satisfy mass and momentum conservation in the heat wave reference frame.The details of this sequence of events depend, among other things, on the opacity and heat capacity of the surrounding medium. Second shock formation is observed over the entire range from 100% Xe mass fraction to 100% N 2 . The formation radius of the second shock as a function of Xe mass fraction is consistent with an analytical estimate.

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Section: Introductionmentioning

confidence: 99%

Secondary shock formation in xenon-nitrogen mixtures

et al. 2006

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“…They have observed structure in radiative blast waves [24][25][26] in Xe gas at ϳ10 km/ s and ϳ10 −5 g / cm 3 . They have diagnosed in detail the radiative precursor ahead of such shocks in Xe gas [27][28][29][30][31] at ϳ50 km/ s and ϳ10 −3 g / cm 3 or in SiO 2 foams. 32 They have diagnosed the structure and dynamics of the shocked material [33][34][35][36][37][38] in Xe gas at ϳ150 km/ s and ϳ10 −2 g / cm 3 .…”

Section: Strong Shocks and Radiative Shocksmentioning

confidence: 99%

Perspectives on high-energy-density physics

2009

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Much of 21st century plasma physics will involve work to produce, understand, control, and exploit very nontraditional plasmas. High-energy-density (HED) plasmas are often examples, variously involving strong Coulomb interactions and ⪡1 particles per Debye sphere, dominant radiation effects, and strongly relativistic or strongly quantum-mechanical behavior. Indeed, these and other modern plasma systems often fall outside the early standard theoretical definitions of “plasma.” Here the specific ways in which HED plasmas differ from traditional plasmas are discussed. This is first done by comparison of important physical quantities across the parameter regime accessible by existing or contemplated experimental facilities. A specific discussion of some illustrative cases follows, including strongly radiative shocks and the production of relativistic, quasimonoenergetic beams of accelerated electrons.

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“…Radiative precursors have been observed in experiments by Bozier et al, 38 Grun et al, 39 Keiter et al, 37 and Koenig, Bouquet, and coworkers. [40][41][42][43][44][45][46] The experiment of Grun et. al.…”

Section: Radiative Shocks a Importance Of The Workmentioning

confidence: 99%

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

Drake¹

2007

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Target for a supernova hydrodynamics experiment. The large acrylic shield has several advantages.Dual orthogonal backlit pinhole radiographs using ungated detectors. From experiments to study Rayleigh-Taylor evolution from a 3D sinusoidal pattern, at 21 ns. Left: an image across the CHBr strip. Right: an image down the CHBr strip. In both images dense spikes and the shockwave can be seen. They are moving to the right. The grid is for spatial calibration and magnification. The bright white feature on the left is a scratch on the film. Radiograph, of radiative shock in Xe gas after image processing to remove x-ray intensity variations.

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A laser experiment for studying radiative shocks in astrophysics

Cited by 51 publications

References 8 publications

Secondary shock formation in xenon-nitrogen mixtures

Secondary shock formation in xenon-nitrogen mixtures

Perspectives on high-energy-density physics

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

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