Coronal heating and emission mechanisms in AGN
| dc.creator | Di Matteo, Tiziana | |
| dc.date | 1999-12-10 | |
| dc.date.accessioned | 2026-07-07T02:34:55Z | |
| dc.date.available | 2026-07-07T02:34:55Z | |
| dc.description | 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. | |
| dc.description | 10 pages, to appear in the proceedings of the Bologna conference on "X-ray Astronomy 1999: Stellar Endpoints, AGN, and the Diffuse X-ray Background" (Astroph. Lett. and Comm.) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9912221 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9912221 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/15432 | |
| dc.subject | Astrophysics | |
| dc.title | Coronal heating and emission mechanisms in AGN | |
| dc.type | text |