Other
Scientific paper
Sep 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...332..842b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 332, Sept. 15, 1988, p. 842-856.
Other
5
Astronomical Models, Conductive Heat Transfer, Supernova Remnants, Supernovae, Interstellar Chemistry, Shock Wave Interaction, Stellar Envelopes, Stellar Winds
Scientific paper
Chevalier's (1982) work on adiabatic self-similar solutions for a supernova envelope expanding into a stationary medium is generalized here to cases with heat transport. Interaction regions which are isothermal, isentropic, or modified by saturated heat conduction are considered. For an isothermal, or isentropic interaction region formed by a given envelope and medium, a family of solutions exists, parameterized by the temperature or entropy, respectively. In no case do energy-conserving solutions exist. While the equations for an interaction region with saturated heat conduction can be written in self-similar form, there are no physical solutions. It is found that heat conduction transfers energy from the shocked medium to the shocked ejecta, decreasing the distance from the forward shock to the contact surface and increasing the distance from the contact surface to the reverse shock. In the isentropic and isothermal solutions, the maximum jump at the reverse shock limits the temperature behind the shock.
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