Computer Science – Numerical Analysis
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45..775n&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan, vol. 45, no. 6, p. 775-787
Computer Science
Numerical Analysis
31
Accretion Disks, Active Galactic Nuclei, Quasars, Stellar Coronas, X Ray Spectra, Monte Carlo Method, Numerical Analysis, Spectral Emission
Scientific paper
A model for the central engine of active galactic nuclei (abbreviated as AGN) has been constructed to simultaneously explain their UV bump and X-ray spectra. It is based on an accretion disk model around a supermassive black hole in that a cold optically thick disk is surrounded by a hot 'corona' and that energy dissipation is supposed to occur mainly in the hot corona, a model along the line proposed by Haardt and Maraschi (1991). It is shown that such a model can be constructed self-consistently within the framework of the standard accretion disk theory under the assumptions that an alpha model for the viscosity parameter is adopted to be applicable simultaneously to the cold disk and the hot corona and that the cold disk and the hot corona are strongly coupled so that they are simultaneously accreted onto the central black hole. All physical variables, such as the surface density of the cold disk, and the electron temperature and the optical depth of the hot corona, are determined as functions of the radial coordinate r of the disk for a given mass of the central massive black hole and a given mass accretion rate. Theoretical energy spectra of the models were calculated by using Monte Carlo simulations for the inverse Compton scattering by thermal electrons in the hot corona; they were found to be in a fairly good agreement with the observed spectra in AGN. It is shown that this model can avoid most of instabilities to which most of other AGN accretion disk models suffer.
Nakamura Kaori
Osaki Yoji
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