Recent results from observations of black hole X-ray binaries are
inconsistent with existing spectral models of accretion disks. The models
are unable to reproduce the observed trends in color temperature with
luminosity. I will summarize these results and discuss our efforts to
develop a sophisticated spectral model with a more accurate treatment of
radiative transfer. I will demonstrate how our models are consistent with
the observations and provide preliminary fitting results. I will also
discuss numerical simulations of the radiation-magnetohydrodynamics of
accretion disks and our initial efforts to incorporate the results of
these calculations into our spectral models.
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