  We present numerical calculations of spectra and structure of accretion disks
models appropriate for near-Eddington luminosity black hole X-ray binaries
(BHB). Our work incorporates non-zero torque at the ISCO as well as several
dissipation profiles based on first-principles three-dimensional disk interior
simulations. We found that significant dissipation near the photosphere can
produce steep power law-like spectra for models with moderate viewing angles
spanning a range of black hole spins while including inner torque push the
spectral peak to higher energies. Consistent with previous studies, we also
conclude that disks with stresses at the inner edge remain viable models for
high-frequency quasi-periodic oscillations (HFQPO), especially given that
increasing dissipation near the photospheres actually resulted in QPO power
spectra with higher quality factors compared to those found in recent work.
