Abstract
We show that the model proposed by Esin, McClintock, & Narayan for the low state, intermediate state, and high state of the black hole soft X-ray transient, Nova Muscae 1991, is consistent with the spectral evolution of the black hole X-ray binary, Cyg X-1, during the hard-to-soft state transition observed in 1996. We also apply the model to the outbursts of two other black hole X-ray transients, GRO J0422+32 and GRO J1719-24.
Highlights
Galactic X-ray sources that contain accreting black holes are among the most interesting objects in high energy astrophysics
We show that the data are consistent with the basic scenario described above, namely that during the transition Cyg X-1 went from the low state, with a relatively large inner radius for the thin disk and an accretion rate near the critical value, to a series of intermediate states with smaller transition radii, and culminated in the high state with Rtr = 3RSchw
We demonstrate that the spectrum of GRO J0422+32 near the peak of the outburst is well modeled by a low state spectrum with m ∼ mcrit
Summary
Galactic X-ray sources that contain accreting black holes are among the most interesting objects in high energy astrophysics. We show that the data are consistent with the basic scenario described above, namely that during the transition Cyg X-1 went from the low state, with a relatively large inner radius for the thin disk and an accretion rate near the critical value, to a series of intermediate states with smaller transition radii, and culminated in the high state with Rtr = 3RSchw. We show that this model convincingly explains the overall spectral evolution of the system, as well as reproduces its hard and soft state spectra fairly well.
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