Aspherical Supernova Shock Breakout and the Observations of Supernova 2008D

Details Aspherical Supernova Shock Breakout and the Observations of Supernova 2008D Aspherical Supernova Shock Breakout and the Observations of Supernova 2008D

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543003c&link_type=abstract

American Astronomical Society, AAS Meeting #215, #430.03; Bulletin of the American Astronomical Society, Vol. 42, p.356

Astronomy and Astrophysics

Astronomy

Scientific paper

Supernova 2008D was discovered on 9 January 2008 during follow up observations of SN 2007uy with the {\it Swift} telescope. The supernova was first identified as a bright X-ray flash lasting approximately 600 seconds. Despite observations of unprecedented detail, the exact mechanism that gave rise to the X-ray outburst is unclear. X-ray emission mechanisms involving scattering of electrons to high energies require the existence of a thin, fast shock. Such a shock may not exist as the supernova shock erupts from the surface of the progenitor due to radiative pre-acceleration of unshocked material. Simple black-body emission models of the burst fail to match the shape of the X-ray spectrum as well as power-law spectra and suffer from an inability to account for the time scale of the burst. For a Wolf-Rayet progenitor, the length of the X-ray burst arising from the thermal emission of a shock breakout would be about 20-30 seconds, while the X-ray burst associated with SN 2008D lasted approximately 120 seconds. We present high-resolution, long time scale numerical simulations of aspherical supernovae in helium star progenitors. We demonstrate the significant differences between the emission properties of spherical and aspherical shock breakouts. We show that, for thermal emission, the time scale of the X-ray burst is not the light travel time across the progenitor surface, but rather the longer shock crossing time of the progenitor surface. Additionally, the thermal spectra produced by aspherical shock breakouts cannot be characterized by a single color temperature at any time. We compare the results of our numerical models to the observations of SN 2008D.

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