Reverse Radiative Shock Experiments Relevant to Accreting Stream-Disk Impact in Interacting Binaries

Details Reverse Radiative Shock Experiments Relevant to Accreting Stream-Disk Impact in Interacting Binaries Reverse Radiative Shock Experiments Relevant to Accreting Stream-Disk Impact in Interacting Binaries

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21813407k&link_type=abstract

American Astronomical Society, AAS Meeting #218, #134.07; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astrophysics

Scientific paper

In many Cataclysmic Binary systems, mass onto an accretion disk produces a `hot spot’ where the infalling supersonic flow obliquely strikes the rotating accretion disk. This collision region has many ambiguities as a radiation hydrodynamic system, but shock development in the infalling flow can be modeled. Depending upon conditions, it has been argued (Armitage & Livio, ApJ 493, 898) that the shocked region may be optically thin, thick, or intermediate, which has the potential to significantly alter the hot spot's structure and emissions.
We report the first experimental attempt to produce colliding flows that create a radiative reverse shock at the Omega-60 laser facility. Obtaining a radiative reverse shock in the laboratory requires producing a sufficiently fast flow (> 100 km/s) within a material whose opacity is large enough to produce energetically significant emission from experimentally achievable layers. We will discuss the experimental design, the available data, and our astrophysical context.
Funded by the NNSA-DS and SC-OFES Joint Prog. in High-Energy-Density Lab. Plasmas, by the Nat. Laser User Facility Prog. in NNSA-DS and by the Predictive Sci. Acad. Alliances Prog. in NNSA-ASC, under grant numbers are DE-FG52-09NA29548, DE-FG52-09NA29034, and DE-FC52-08NA28616.

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