The thermal-viscous disk instability model in the AGN context

Details The thermal-viscous disk instability model in the AGN context The thermal-viscous disk instability model in the AGN context

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..297h&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Physics

1

Scientific paper

Accretion discs in AGN should be subject to the same type of instability as in cataclysmic variables (CVs) or in LMXBs, which leads to dwarf novae outbursts and soft X-ray transients. It has been suggested that this thermal/viscous instability can account for long term variability of AGNs. Using our adaptative grid numerical code developed in the context of CVs, we show that, because the Mach number is very large in AGNs, the width of the heating and cooling fronts is so small that they cannot be resolved by standard codes, and that they propagate on time scales much smaller than the viscous time. As a result, a sequence of heating and cooling fronts propagate back and forth in the disc, leading to small variations of the accretion rate onto the black hole. Truncation of the inner part of the disc by e.g. an ADAF does not alter this result. We finally discuss on the possible effects of irradiation by the central X-ray source.

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