What the R-Gamma correlation tells us about geometry and physical processes in accreting black hole sources

Details What the R-Gamma correlation tells us about geometry and physical processes in accreting black hole sources What the R-Gamma correlation tells us about geometry and physical processes in accreting black hole sources

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aax..proc...69m&link_type=abstract

Atelier d'astronomie X, X-ray Astronomy workshop, held in Toulouse (France), September 20, 2000, Eds. J. Ballet (jballet@cea.fr)

Astronomy and Astrophysics

Astronomy

Scientific paper

We discuss the spectral properties of Seyfert galaxies, and galactic black hole candidates, in the hard X-ray domain. We focus on the information brought by the observed correlation between the spectral slope Gamma and the amplitude of the reflection component R. This correlation suggests that both the soft seeds photons of the Comptonisation process, and the reflection component originate from the same cold medium. Based on this assumption, several models have been proposed, that may account for the correlation. We show that accurate radiative transfer calculations and energy balance arguments, together with good quality data, can put some constraints and help in discriminating between them. We focus on 4 possible models: (i) the hot inner disc model, (ii) the inhomogeneous plasma, (iii) the spherical inner accretion flow, (iv) the dynamic corona. Our conclusions are the following: (i) the usual inner hot disk model is not able to reproduce the correlation observed in Seyferts, and meet important dificulties in galactic sources, (ii) the soft photon/reflection source cannot be mixed inside the hot Comptonising plasma. The hot and cold phase are clearly separated. (iii) the spherical accretion scenario, as well as (iv) the dynamic corona model are in good agreement with the data.

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