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Abteilung Astronomie

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Preprint 13b/96

Properties of Accretion Disk Coronae

J. Wilms(1), J. Dove(2), R. Staubert(1), M. C. Begelman(2)

(1)Institut für Astronomie und Astrophysik, Astronomie, Universität Tübingen, Waldhäuser Str. 64, D-72076 Tübingen, Germany
(2)JILA, University of Colorado, Campus Box 440, Boulder, CO 80309-0440, U.S.A.

Contribution to the Conference The Transparent Universe - 2nd Integral Symposium, St. Malo, France, September 16-20, 1996
to be published in the Proceedings of this Conference

Abstract. We present results on the properties of accretion disk coronae in a parameter regime suitable for galactic black hole candidates computed using a self-consistent Monte Carlo code. We present examples of the coronal temperature structure, the shape and angular dependency of the spectrum, and the maximum temperature allowed for each optical depth of the corona. We show that the observed spectrum of the galactic black hole candidate Cygnus X-1 can not be explained by accretion disk corona models having a slab geometry, where the accretion disk is sandwiched by the comptonizing medium.

Key words: Accretion disks; Comptonization; X-ray binaries; Cygnus X-1

Paper (49k gzip'ed Postscript including figures)

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Jürgen Barnstedt (barnstedt AT astro.uni-tuebingen.de)
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