Hydrodynamics of Supernova Evolution in the Winds of Massive Stars
Abstract
Description
Core-Collapse supernovae arise from stars greater than 8 $\msun$. These stars lose a considerable amount of mass during their lifetime, which accumulates around the star forming wind-blown bubbles. Upon the death of the star in a spectacular explosion, the resulting SN shock wave will interact with this modified medium. We study the evolution of the shock wave, and investigate the properties of this interaction. We concentrate on the evolution of the SN shock wave in the medium around a 35 solar mass star. We discuss the hydrodynamics of the resulting interaction, the formation and growth of instabilities, and deviations from sphericity.
11 pages, 4 figures. Accepted to Astrophysics and Space Science. To be published by Springer in special volume of the High Energy Density Lab Astrophysics Conference #6. For a version with higher resolution figures see http://astro.uchicago.edu/~vikram/sncirc/vikram_2.pdf
11 pages, 4 figures. Accepted to Astrophysics and Space Science. To be published by Springer in special volume of the High Energy Density Lab Astrophysics Conference #6. For a version with higher resolution figures see http://astro.uchicago.edu/~vikram/sncirc/vikram_2.pdf