Optically thin accretion disks in the Kerr metric

Details Optically thin accretion disks in the Kerr metric Optically thin accretion disks in the Kerr metric

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...441..765b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 441, no. 2, p. 765-769

Astronomy and Astrophysics

Astronomy

6

Accretion Disks, Angular Momentum, Astronomical Models, Black Holes (Astronomy), Optical Thickness, Bremsstrahlung, Electron-Positron Pairs, Mathematical Models, Relativistic Effects, Relativity

Scientific paper

We calculate the structure of an effectively optically thin and geometrically thin accretion disk in the Kerr geometry, including electron-positron pairs. We show that the properties of the disk solutions are strongly dependent on the angular momentum of the central black hole. We find that close to a rapidly rotating hole there can be an appreciable pair density even for modest accretion rates. Pair critical accretion rates recently discovered in Newtonian disk models are also shown to be present in the general relativistic models, and we show that the geometrically thin disk approximations easily break down for rapidly rotating holes.

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