Supernovae in Dense Winds

Details Supernovae in Dense Winds Supernovae in Dense Winds

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..401..185c&link_type=abstract

RS Ophiuchi (2006) and the Recurrent Nova Phenomenon ASP Conference Series, Vol. 401, proceedings of the conference held 12-14 J

Astronomy and Astrophysics

Astronomy

Scientific paper

The ejecta of a massive star supernova initially interact with the wind from the progenitor star. A self-similar flow is set up with a shocked region bounded by forward and reverse shock waves. This hydrodynamic picture provides a context for understanding multiwavelength observations of supernovae: nonthermal radio emission, thermal X-ray emission, optical emission from radiative shocks and photoionized gas, and dust emission. Although the hydro-dynamic situation is different in the case of the outburst of RS Oph, the fact that the shock velocities and gas densities are similar implies that similar physical processes occur in these two cases.

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