Radiative Shocks with Dense Post-Shock Layers at the Omega Laser

Details Radiative Shocks with Dense Post-Shock Layers at the Omega Laser Radiative Shocks with Dense Post-Shock Layers at the Omega Laser

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21641003d&link_type=abstract

American Astronomical Society, AAS Meeting #216, #410.03; Bulletin of the American Astronomical Society, Vol. 41, p.817

Astronomy and Astrophysics

Astrophysics

Scientific paper

Astrophysical systems in which radiation transport across a shock front contributes substantially to the properties and dynamics of the system may in certain respects be modeled in laboratory experiments under high-energy-density conditions. A series of experiments on the Omega Laser Facility have launched beryllium discs into shock tubes of xenon gas at atmospheric pressure, producing radiative shocks with optically thin precursors and speeds over 100 km/sec. These shocks are primarily diagnosed by x-ray pinhole radiography.
These experiments are found to develop rich internal structure. First, radiative losses lead to a very high compression of the shocked fluid and the formation of a dense post-shock layer. Second, these radiating, decelerating shock systems become susceptible to hydrodynamic instabilities of thin shocked layers. Third, heating and ablation of the shock tube material ahead of the radiative shock drives a secondary, inwardly directed radial shock, which we call a wall shock.
The governing equations of these effects are subject to scaling relations which establish similarity between their appearances in these experiments and under astrophysical conditions. In some experiments it may be possible to establish similarity of the smaller length and time scales of the second effect even when the larger scales of the overall dynamics cannot be so scaled.
This work is funded by the DOE NNSA-DS and SC-OFES Joint Program in High-Energy-Density Laboratory Plasmas by grant DE-FG52-09NA29548, by the National Laser User Facility Program in NNSA-DS by grant DE-FG52-09NA29034, by the Predictive Sciences Academic Alliances Program in NNSA-ASC by grant DE-FC52-08NA28616, and by the DOE Stewardship Science Graduate Fellowship program.

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