Shock Breakout Emission from a Type Ib/c Supernova: XRT 080109/SN 2008D

TL;DR

This paper investigates the shock breakout emission in Type Ib/c supernovae, explaining observed X-ray and optical features with models that align with stellar evolution, and discusses the implications for specific supernovae including SN 2008D.

Contribution

The study develops a simple model for shock breakout emission and applies it to multiple supernovae, providing insights into their progenitor star properties and emission mechanisms.

Findings

X-ray flash 080109 is consistent with shock breakout emission.

Optical/UV emission at ~1 day can be attributed to shock breakout in several supernovae.

Early observations of SN 2006aj challenge simple shock breakout explanations.

Abstract

The X-ray flash 080109, associated with SN 2008D, can be attributed to the shock breakout emission from a normal Type Ib/c supernova. If the observed emission is interpreted as blackbody emission, the temperature and radiated energy are close to expectations, considering that scattering dominates absorption processes so that spectrum formation occurs deep within the photosphere. The X-ray emission observed at ~10 days is attributed to inverse Compton scattering of photospheric photons with relativistic electrons produced in the interaction of the supernova with the progenitor wind. A simple model for the optical/ultraviolet emission from shock breakout is developed and applied to SN 1987A, SN 1999ex, SN 2008D, and SN 2006aj, all of which have optical emission observed at t~1 day. The emission from the first three can plausibly be attributed to shock breakout emission. The photospheric temperature is most sensitive to the radius of the progenitor star core and the radii in these cases are in line with expectations from stellar evolution. The early optical/ultraviolet observations of SN 2006aj cannot be accommodated by a shock breakout model in a straightforward way.