The evolution of the optically thick accretion disk in nova muscae

We here model the soft X-ray flux from the black hole X-ray nova, GS 1124-68 (Nova Muscae, GRS 1124-68) as emission from an optically thick accretion disk with Comptonization. Our results suggest that the disk's inner edge has a radius the dependence of which on the accretion rate is a power law, and that the slope of this function changes between the different spectral states. This disk configuration retains a hot inner region, which can account for the hard X-rays, although its structure appears to be different during the soft and ultra-soft states.