Understanding the long-term spectral variability of Cygnus X-1 with BATSE and ASM observations

Details Understanding the long-term spectral variability of Cygnus X-1 with BATSE and ASM observations Understanding the long-term spectral variability of Cygnus X-1 with BATSE and ASM observations

2002-04-08

arxiv.org/abs/astro-ph/0204135v2

Astrophys.J.578:357-373,2002

Astronomy and Astrophysics

Astrophysics

ApJ, in press (the final version after referee's comments), 26 pages, needs to be printed in color

Scientific paper

10.1086/342402

We present an analysis of all observations of Cygnus X-1 by the BATSE (20-300 keV) and by ASM (1.5-12 keV) until 2002 June, including 1200 days of simultaneous data. We find a number of correlations between fluxes and hardnesses in different energy bands. In the hard state, the variability can be explained by softening the overall spectrum with a pivot at 50 keV and another, independent variability pattern where the spectral shape does not change when the luminosity changes. In the soft state, the variability is caused by a variable hard tail of a constant shape superimposed on a constant soft component. These variability patterns are in agreement with the energy-dependent rms variability in the two states. We also study in detail recent soft states in 2000-02. The last of them has lasted so far for >200 days. Their spectra are harder in the 1.5-5 keV band but similar or in the 3-12 keV band than those of the 1996 soft state whereas the rms variability is stronger in all the ASM bands. On the other hand, the 1994 soft state transition observed by BATSE appears very similar to the 1996 one. We interpret the variability patterns by theoretical Comptonization models. In the hard state, the variability appears to be driven mostly by changing flux in seed photons Comptonized in a hot thermal plasma cloud with an approximately constant power supply. In the soft state, the variability is consistent with flares of hybrid, thermal/nonthermal, plasma with variable power above a stable cold disk. The spectral and timing differences between the 1996 and 2000-02 soft states are explained by a decrease of the color disk temperature. Also, based on broad-band pointed observations, we find the intrinsic bolometric luminosity increases by a factor of 3-4 from the hard state to the soft one.

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