Accretion disc coronae in black hole binaries

Details Accretion disc coronae in black hole binaries Accretion disc coronae in black hole binaries

2007-07-11

arxiv.org/abs/0707.1612v1

Mem.Soc.Ast.It.78:382,2007

Astronomy and Astrophysics

Astrophysics

8 pages, 1 figure; invited review at the 'Coronae of Stars and Accretion Disks' conference, Bonn, 12-13 December 2006

Scientific paper

Most of the luminosity of accreting black hole is emitted in the X-ray band. This radiation is believed to emerge, through inverse Compton process, from a hot (Te ~ 10^8 -10^9 K) optically thin (Thomson optical depth ~ 1) plasma probably located in the immediate vicinity of the black hole. The mechanisms at work in this so called Compton corona can be unveiled through hard X-ray observations which have revealed a rich phenomenology. Depending on luminosity different spectral states are observed suggesting that the nature and geometry of the corona depends on mass accretion rate. In many instances the spectral behaviour as a function of luminosity shows some degree of hysteresis. The mechanisms triggering the transition between spectral states is very unclear although it could be related to an evaporation/condensation equilibrium in an accretion disc corona system. From the observation of correlation between the X-ray and radio band, it appears that the Compton corona is intimately related to the formation of compact jets and probably constitutes the base of the jet.

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