Formation of supernova remnants - The pre-blast-wave phase

Details Formation of supernova remnants - The pre-blast-wave phase Formation of supernova remnants - The pre-blast-wave phase

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...249..185j&link_type=abstract

Astrophysical Journal, Part 1, vol. 249, Oct. 1, 1981, p. 185-194. Research supported by the U.S. Department of Energy

Astronomy and Astrophysics

Astrophysics

69

Hydrodynamics, Shock Waves, Stellar Evolution, Stellar Structure, Supernova Remnants, X Ray Sources, Computerized Simulation, Density Distribution, Gravitational Collapse, Interstellar Matter, Stellar Mass, Stellar Models, Taylor Instability

Scientific paper

The effect of stellar structure on supernova remnant formation is studied with a series of computer models of a 10 to the 51st erg explosion in a 15 solar mass star. Immediately after the explosion shock wave travels down a steep density gradient, the material in the gradient goes into free expansion, forming a collapsible piston. At the outer edge of such a piston are two shock waves: the expanding supernova shock and a reverse shock moving back into the collapsible piston. Until the piston is completely collapsed it is Rayleigh-Taylor stable, but after collapse the inner material behaves as a massive piston and the interface is Rayleigh-Taylor unstable. If there is a significant mass in an external density gradient, the material between the supernova shock moving out through the interstellar medium and the reverse shock will be a significant source of X-rays during the pre-blast-wave phase of remnant formation.

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