Coronal heating and emission mechanisms in AGN

Details Coronal heating and emission mechanisms in AGN Coronal heating and emission mechanisms in AGN

1999-12-10

arxiv.org/abs/astro-ph/9912221v1

Astronomy and Astrophysics

Astrophysics

10 pages, to appear in the proceedings of the Bologna conference on "X-ray Astronomy 1999: Stellar Endpoints, AGN, and the Dif

Scientific paper

Popular models for the formation of X-ray spectra in AGN assume that a large fraction of the disk's angular momentum dissipation takes place in a hot corona that carries a small amount of the accreting mass. Here I discuss the formation of a magnetically-structured accretion disk corona, generated by buoyancy instability in the disk and the heating of localized flare regions up to the canonical X-ray emitting temperatures. I also examine the analogy between accreting disk-coronae and ADAFs and discuss the relevant emission mechanism in these two accretion models and how observational constraints can allow us to discriminate between them.

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