Super-Eddington fluxes from thin accretion disks?

Radiation pressure-dominated accretion disks are predicted to exhibit strong density inhomogeneities on scales much smaller than the disk scale height as a result of the nonlinear development of photon-bubble instability. Radiation would escape from such a leaky disk at a rate higher than that predicted by standard accretion disk theory. The disk scale height is then smaller than that of a similar disk without small-scale inhomogeneities, and the disk can remain geometrically thin even as the flux approaches and exceeds the Eddington limit. An idealized one-zone model for disks with radiation-driven inhomogeneities suggests that the escaping flux could exceed L-Edd by a factor of up to similar to10-100, depending on the mass of the central object. Such luminous disks would LEdd develop strong mass loss, but the resulting decrease in accretion rate would not necessarily prevent the luminosity from exceeding L-Edd. We suggest that the observed ultraluminous X-ray sources are actually thin, super-Eddington accretion disks orbiting stellar-mass black holes and need not indicate the existence of a class of intermediate-mass black holes.