We report XMM-Newton observations of the intermediate polar (IP) GK Per on
the rise to the 2002 outburst and compare them to Chandra observations during
quiescence. We find an asymmetric spin light curve implying an asymmetric shape
of a semi-transparent accretion curtain. A low Fe xvii (15.01/15.26 A) line
flux ratio confirms the need for an asymmetric geometry and significant effects
of resonant line scattering. Medium resolution spectra in outburst and
quiescence are both fitted with a leaky absorber model for the post shock hard
X-ray emission, a black body (outburst) for the thermalized X-ray emission from
the white dwarf and an optically thin spectrum. The difference between high and
low spin as well as QPO/flares states can be explained by a variation in the
absorbing column density. The Fe fluorescence at 6.4 keV (equivalent width of
447 eV) is not significantly variable during spin cycle or on QPO periods.
High-resolution RGS spectra reveal a number of emission lines from H-like and
He-like elements. The lines are broader than the instrumental response with a
roughly constant velocity dispersion for different lines, indicating identical
origin. He-like emission lines are used to give values for the electron
densities of log n_e ~ 12. We do not detect any variation in the emission lines
during the spin cycle, implying that the lines are not noticeably obscured or
absorbed. We conclude that they originate in the accretion curtains and propose
a model for their shape.Comment: 14 pages, 22 figures, accepted by A&A; text re quiescent data changed
slightly, references adde