Astronomy and Astrophysics – Astrophysics
Scientific paper
2005-02-21
Mon.Not.Roy.Astron.Soc. 362 (2005) 1435-1450
Astronomy and Astrophysics
Astrophysics
17 pages, 11 figures, accepted to MNRAS. Changes to v2: added N_H notes, improved discussion on timing, new calibration used
Scientific paper
10.1111/j.1365-2966.2005.09415.x
We present the results of spectral analysis of 42 simultaneous broad-band Ginga--OSSE and RXTE--OSSE observations of Cyg X-1 carried out in 1991 and 1996--1999. The hardest spectra in our sample in the energy range from 3 to \~1000 keV can be well described by thermal Comptonization model with reflection from the cold disc, while the rest of the spectra are more complex and require an additional component below 10 keV. We consider a number of physically realistic models to describe the shape of the E<10 keV excess. The additional soft component can result from thermal Comptonization by electrons with a low Compton parameter, or can be a part of a nonthermal, power-law like emission extending above 1 MeV. We study correlations between parameters obtained from the spectral fits with different models. We confirm a general correlation between the photon index $\Gamma$ and the amplitude of reflection R. We find that simple phenomenological models (like power-law plus Compton reflection) applied to the narrow band (3--20 keV) data overestimated the values of R and $\Gamma$, although the simple models did rank correctly the spectra according to R and $\Gamma$. The dynamic corona model provides a satisfactory description of the observed correlation, while the hot inner disc models have problems in reproducing it quantitatively. We do not find significant correlation between the electron temperature and other spectral parameters, while the optical depth of the hot medium seems to decrease when the spectrum becomes softer. It is also shown that spectral parameters are well correlated with the timing characteristics of the source.
Gilfanov Marat
Ibragimov A. A.
Poutanen Juri
Shrader Chris R.
Zdziarski Andrzej A.
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