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Session 12 - Degenerate Stars & Supernovae.
Oral session, Monday, June 09
North Main Hall C/D,

[12.07] SNR Evolution Through a Realistic Circumstellar Medium

V. Rekovic (Guilford College), J. Blondin, S. Reynolds (NCSU)

Massive progenitor stars of type II supernovae change their environments through powerful stellar winds that deplete perhaps up to 80% of the original mass of the star. The properties of the wind can vary drastically as the star evolves across different regions of the HR diagram. As a consequence, a highly structured circumstellar bubble around the star is created. Type II supernovae therefore occur in a complex, modified environment rather than in a uniform medium as is often assumed. In the first part of this paper we present a one-dimensional hydrodynamical simulation to model the development of a circumstellar bubble around a 60 solar mass star. The evol ution of the bubble expanding in a uniform ambient medium with constant density is followed until the end of the star's life - a type II supernova. In the second part, we present a one dimensional hydrodynamical simulation for the evolution of a supernova remnant surrounded by the circumstellar bubble discussed in part one. We initialize the SNR as a self-similar driven wave in the immediate undisturbed stellar wind of the progenitor star. Subsequent evolution of the SNR is compared with the standard assumption of self-similar evolution, as in the Sedov-Taylor solution.

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