TIME-DEPENDENT DISK ACCRETION IN X-RAY NOVA MUSCAE 1991

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We propose a new model for X-ray spectral fitting of binary black hole candidates. In this model, it is assumed that X-ray spectra are composed of a Comptonized blackbody (hard component) and a disk blackbody spectra (soft component), in which the temperature gradient of the disk, q = -d log T/d log r, is left as a fitting parameter. With this model, we have fitted X-ray spectra of X-ray Nova Muscae 1991 obtained by Ginga. The fitting shows that a hot cloud, which Compton up-scatters soft photons from the disk, gradually shrank and became transparent after the main peak. The temperature gradient turns out to be fairly constant and is q ~ 0.75, the value expected for a Newtonian disk model. To reproduce this value with a relativistic disk model, a small inclination angle, i ~ 0°-15°, is required. It seems, however, that the q-value temporarily decreased below 0.75 at the main flare, and q increased in a transient fashion at the second peak (or the reflare) occurring ~70 days after the main peak. Although statistics are poor, these results, if real, would indicate that the disk brightening responsible for the main and secondary peaks are initiated in the relatively inner portions of the disk.

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