  We present numerical spectral and vertical structure calculations appropriate
for near-Eddington-luminosity, radiation-pressure-dominated accretion disks
around stellar-mass black holes. We cover a wide range of black hole spins and
incorporate dissipation profiles based on first-principles three-dimensional
MHD disk interior simulations. We also include nonzero stresses at the
innermost stable circular orbit, which results in the disk effective
temperature increasing rapidly toward the black hole and gives rise to rather
extreme conditions with high temperatures and low surface densities. We found
that local annulus spectra become increasingly characteristic of saturated
Comptonization with decreasing distance to the black hole. While the spectra
become harder with increasing black hole spin, they do not give rise to a broad
power-law tail even at maximum spin. We discuss the implications of our results
in the context of the steep power-law state and the associated high-frequency
quasi- periodic oscillations observed in some X-ray binary systems.
