Abstract
We discuss constraints on the physics of the inner accretion disk, as well as the properties of the black hole itself, that can be derived by a detailed examination of the relativistically broadened spectral features (especially the fluorescent iron line) in the Seyfert galaxy MCG-6-30-15. To begin with, we show that spectral models which purport to eliminate the broad iron line in MCG-6-30-15 by invoking a moderately high ionization absorber are ruled out by recent high-resolution spectra from the Chandra High Energy Transmission Gratings. We then discuss the comparison of XMM-Newton data with accretion disk models. The ``standard'' black hole disk model of Novikov, Page and Thorne supplemented by the so-called local corona assumption fails to produce sufficient broadening; this indicates that the real accretion disk in MCG-6-30-15 has significantly more centrally concentrated pattern of X-ray irradiation that predicted by this model. We discuss two possible resolutions. Firstly, the inner disk may be energized from torques imposed by magnetic connections between the disk-proper and either the plunging region or the rotating event horizon itself. Secondly, X-ray emission from a high-latitude source (such as would be the case if the X-ray source is actually the base of a jet) would be gravitationally focused onto the central portions of the disk. We discuss how spectral variability may be used to examine these possibilities and highlight the still outstanding mystery concerning the anti-correlation between the iron line equivalent width and relative normalization of the Compton reflection hump. We end with a few words about the exciting future of these studies heralded by Constellation-X and LISA.
