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We present numerical spectral and vertical structure calculations appropriatefor near-Eddington-luminosity, radiation-pressure-dominated accretion disksaround stellar-mass black holes. We cover a wide range of black hole spins andincorporate dissipation profiles based on first-principles three-dimensionalMHD disk interior simulations. We also include nonzero stresses at theinnermost stable circular orbit, which results in the disk effectivetemperature increasing rapidly toward the black hole and gives rise to ratherextreme conditions with high temperatures and low surface densities. We foundthat local annulus spectra become increasingly characteristic of saturatedComptonization with decreasing distance to the black hole. While the spectrabecome harder with increasing black hole spin, they do not give rise to a broadpower-law tail even at maximum spin. We discuss the implications of our resultsin the context of the steep power-law state and the associated high-frequencyquasi- periodic oscillations observed in some X-ray binary systems.

Spectra and Structure of Accretion Disks with Nonzero Inner Torque