Shock Waves in Supernova Ejecta
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Astrophysical shock waves are a major mechanism for dissipating energy, and by heating and ionizing the gas they produce emission spectra that provide valuable diagnostics for the shock parameters, for the physics of collisionless shocks, and for the composition of the shocked material. Shocks in SN ejecta in which H and He have been burned to heavier elements behave differently than shocks in ordinary astrophysical gas because of their very large radiative cooling rates. In particular, extreme departures from thermal equilibrium among ions and electrons and from ionization equilibrium may arise. This paper discusses the consequences of the enhanced metal abundances for the structure and emission spectra of those shocks.
KeywordsSupernova Shock waves Supernova remnants
This work was supported by GO grant HST-GO-13436.01-A from the Space Telescope Science Institute and by the International Space Sciences Institute. It grew out of the ISSI meeting on Supernovae in October, 2016.
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