  Supernova (SN) 2008D/XRT 080109 is considered to be the only direct detection
of a shock breakout from a regular SN to date. While a breakout interpretation
was favored by several papers, inconsistencies remain between the observations
and current SN shock breakout theory. Most notably, the duration of the
luminous X-ray pulse is considerably longer than expected for a spherical
breakout through the surface of a type Ibc SN progenitor, and the X-ray
radiation features, mainly its flat spectrum and its luminosity evolution, are
enigmatic. We apply a recently developed theoretical model for the observed
radiation from a Wolf-Rayet SN exploding through a thick wind and show that it
naturally explains all the observed features of SN 2008D X-ray emission,
including the energetics, the spectrum and the detailed luminosity evolution.
We find that the inferred progenitor and SN parameters are typical for an
exploding Wolf-Rayet. A comparison of the wind density found at the breakout
radius to the density at much larger radii, as inferred by late radio
observations, suggests an enhanced mass loss rate taking effect about ten days
or less prior to the SN explosion. This finding joins accumulating evidence for
a possible late phase in the stellar evolution of massive stars, involving
vigorous mass loss a short time before the SN explosion.
