NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-18 T23:49:31 PDT
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For refcode 2000NewA....5...69C:
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2000NewA....5...69C On the radial dependence of the disk FeK{alpha} line emissivity in active galactic nuclei Andrej Cadeza, Massimo Calvani, Claudio Di Giacomo, Paolo Marziani calvani@pd.astro.it Department of Physics, University of Ljubljana, Jadranska 19, 61000 Ljubljana, Slovenia Astronomical Observatory, Vicolo Osservatorio 5, 35122 Padova, Italy Department of Physics, University of Padova, Via Marzolo 8, 35131, Padova, Italy Received 27 July 1999; received in revised form 12 February 2000; accepted 24 February 2000 Abstract The iron K{alpha} fluorescent line detected in many Seyfert 1 galaxies by ASCA and BeppoSAX is usually considered to arise in the innermost region of an accretion disk around a supermassive black hole. The line profile is usually modelled by assuming that the disk emissivity follows a power law, {epsilon}(R) is proportional to R^-4^. We present a new technique to invert the line profile and infer: (a) the free-format {epsilon}(R), (b) the disk inclination to the line of sight and (c) the black hole angular momentum. The application of this technique to published K{alpha} data shows that the line shapes are consistent with the accretion disk model and that the major contribution to the emissivity comes from the innermost disk regions. We also show that a sharp distinction between different black hole angular momenta can usually not be made on the basis of present data. Keywords: Accretion, accretion disks; Black hole physics; Galaxies: active; Galaxies: nuclei; X-rays: galaxies
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