Summary:
ÿ XMM spectra consistent with obscuration
model by a precessing disk
ÿ Low State identified with illuminated
accretion disk atmosphere and 
hot corona from high resolution
spectroscopy.
hot corona from high resolution
spectroscopy. ÿ Detection of a Fe line at 7 keV during
the low state: signature of the hottest layers of the corona
hottest layers of the corona ÿ RGS: narrow line emission during the
low state. Photo ionized layers above
the disk
above
the disk ÿ 35 d variability of the ~6.4 keV Fe line. Emitting
regions probably different
during low and high state.
different
during low and high state. ÿ UV modulation along the orbital period
in both OM filters.
ÿ Before the ALS: spin-down and change in the
hard/soft phase shift Þ was the inner disk changing?
shift Þ was the inner disk changing?ÿ Spectra taken during the ALS remarkably similar to those taken during the
standard low state
the
standard low state