Other
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21533301f&link_type=abstract
American Astronomical Society, AAS Meeting #215, #333.01; Bulletin of the American Astronomical Society, Vol. 42, p.431
Other
Scientific paper
Core-collapse supernovae result in massive explosions that allow us a glimpse of massive stars at the end of their lives. Recently, several supernovae have been observed very close to the initial explosion. The shock wave launched after core collapse breaks out of the stellar surface or dense stellar wind and interacts with the star's immediate surroundings, giving us valuable information about the last stages of stellar evolution. A radiation-hydrodynamics code with adaptive mesh refinement is used to follow the movement of the radiation-dominated shock through shock breakout and wind interactions with high resolution. Using 23 solar mass single and binary progenitors, we study the effects of explosion energy, wind velocity and mass loss history on the X-ray and other radiation generated at shock breakout and beyond. Simulations with the binary progenitor show that the mass loss rate, and so wind density, is the most significant factor in determining the light curve. A dense wind delays and enhances the X-ray burst emitted at shock breakout, as the shock must travel further before reaching an optically thin environment. In the single star, the larger initial radius causes shock breakout to occur near the stellar surface regardless of wind density, and the initial explosion energy has a much larger effect. A lower explosion energy leads to a less luminous, delayed X-ray burst. The effects of these parameters on optical and UV band light curves and specific spectral lines are being studied in more detail.
Frey Lucille
Fryer Chris
Hungerford Aimee
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