Comparison of the solar corona and the coronae above accretion disks surrounding black holes

We develope a model of an accretion disk corona motivated by the observed solar corona. Such a model consists of many unresolved magnetic loops coexisting above the disk surface. We compare the predicted energy-dependent fractional variability amplitude with the observed one, both for standard rms(E) and point-to-point rms(E). Finally, we compare the parameters of a single large flare seen in the lightcurve of MCG -6-15-30 with large solar flares.