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Preprint 12c/99


A. Orr (1;2), G. Torricelli-Ciamponi (3;4), P. Pietrini (5)

(1) Institut für Astronomie und Astrophysik, Astronomie, Universität Tübingen, Waldhäuser Str. 64, D-72076 Tübingen, Germany
(2) Astrophysics Division, ESA/ESTEC, Noordwijk, The Netherlands
(3) Integral Science Data Center, Versoix, Switzerland
(4) Osservatorio Astrofisico di Arcetri, Firenze, Italy
(5) Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, Italy

To appear in: CONFERENCE PROCEEDINGS X-ray Astronomy '99, published in Astrophysical Letters and Communications, 1999,

Abstract. Hot accretion disk coronae may account for substantial X-ray ux in AGN. We present preliminary results from a novel coronal emission model which builds upon the knowledge we have of solar-stellar coronae. The model considers a population of accelerated electrons (such as produced at the onset of a flare) injected at the top of an accretion disk magnetic loop. The inverse Compton and Bremsstrahlung emission for the electron population is computed and compared with AGN X-ray observations. The constraints on model parameters are discussed.

Key words: AGN, corona, accretion disk

Paper (62k gzip'ed Postscript including figures)

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