  Following a CME which started on 2002 November 26, RHESSI, the Ramaty High
Energy Solar Spectroscopic Imager, observed for 12 hours an X-ray source above
the solar limb, at altitudes between 0.1 and 0.3 RS above the photosphere. The
GOES baseline was remarkably high throughout this event. The X-ray source's
temperature peaked around 10-11 MK, and its emission measure increased
throughout this time interval. Higher up, at 0.7 RS, hot (initially >8 MK)
plasma has been observed by UVCS on SoHO for 2.3 days. This hot plasma was
interpreted as the signature of a current sheet trailing the CME (Bemporad et
al. 2006). The thermal energy content of the X-ray source is more than an order
of magnitude larger than in the current sheet. Hence, it could be the source of
the hot plasma in the current sheet, although current sheet heating by magnetic
reconnection within it cannot be discounted. To better characterize the X-ray
spectrum, we have used novel techniques (back-projection based and
visibility-based) for long integration (several hours) imaging spectroscopy.
There is no observed non-thermal hard X-ray bremsstrahlung emission, leading to
the conclusion that there is either very little particle acceleration occurring
in the vicinity of this post- are X-ray source, or that either the photon
spectral index would have had to be uncharacteristically (in flare parlance)
high (gamma >= 8) and/or the low-energy cutoff? very low (Ec <= 6 keV).
