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