Testing models of X-ray reflection from irradiated disks

We model the reflected spectrum expected from localized magnetic flares above an ionised accretion disk. We concentrate on the case of very luminous magnetic flares above a standard accretion disk extending down to the last stable orbit, and use a simple parameterisation to allow for an X-ray driven wind. Full disk spectra including relativistic smearing are calculated. When fit with the constant density reflection models, these spectra give both a low reflected fraction and a small line width as seen in the hard spectra from Galactic Black Hole Binaries and Active Galactic Nuclei. We fit our calculated spectra to real data from the low/hard state of Nova Muscae and Cyg X-1 and show that these models give comparable ${\chi }^2$ to those obtained from the constant density reflection models which implied a truncated disk. This explicitally demonstrates that the data are consistent with either magnetic flares above an ionized disk extending down to the last stable orbit around a black hole, or with non-ionized, truncated disks.