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Accreting corona model of the X-ray variability in soft state GBH and AGN

Published online by Cambridge University Press:  01 August 2006

Bożena Czerny  and
Agnieszka Janiuk
Bożena Czerny
Affiliation:
Copernicus Astronomical Center, Bartycka 18,00-716 Warsaw, Poland email: [email protected]
Agnieszka Janiuk
Affiliation:
Copernicus Astronomical Center, Bartycka 18,00-716 Warsaw, Poland email: [email protected] Department of Physics, University of Nevada, Las Vegas, NV89154, [email protected]
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Abstract

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We develop a two-flow model of accretion onto a black hole which incorporates the effect of the local magneto-rotational instability. The flow consists of an accretion disk and an accreting corona, and the local dynamo affects the disk/corona mass exchange. The model is aimed to explain the power spectra of the sources in their soft, disk-dominated states. The local perturbations of the magnetic field in the disk are described as in King et al. (2004) and Mayer & Pringle (2006), but the time-dependent local magnetic field is assumed to affect the local supply of the material to the corona. The accreting corona model can reproduce the broad power spectra of Soft State X-ray binaries and AGN. The model, however, predicts that (i) sources undergoing radiation pressure instability (GRS 1915+105) should have systematically steeper power spectra than other sources, (ii) AGN should have systematically steeper power spectra than GBH. More measurements of power spectra of Soft State sources are clearly needed.

Keywords

Accretionaccretion disks – galaxies: active – X-rays: binaries – X-rays: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 353 - 354
Copyright
Copyright © International Astronomical Union 2007

References

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Mayer, M. & Pringle, J. E. 2006, MNRAS, 368, 379CrossRefGoogle Scholar
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