X-ray spectra from two-phase accretion disks

Details X-ray spectra from two-phase accretion disks X-ray spectra from two-phase accretion disks

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...413..507h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 413, no. 2, p. 507-517.

Astronomy and Astrophysics

Astronomy

389

Accretion Disks, Active Galactic Nuclei, Compton Effect, Electron Energy, Stellar Luminosity, X Ray Spectra, Astronomical Models, Black Body Radiation, Stellar Coronas, X Ray Astronomy

Scientific paper

A model for the X-ray emission from radio-quiet AGNs is considered. The X-rays are produced via inverse Compton (IC) emission in a hot corona embedding a colder accretion disk. Soft thermal photons emitted by the cold layer provide the main source of cooling for the hot electrons in the corona. At the same time, about half of the high-energy photons produced in the corona are effective in heating the underlying dense layers. The local viscous dissipation within the disk is considered negligible. The energy coupling between the disk and the corona forces the electron temperature to adjust so as to maintain comparable luminosities in the soft and hard components of the emitted radiation, independently of the optical depth of the scattering medium. The coronal equilibrium temperature, as well as the resulting high-energy spectra, are computed taking into account the anisotropy of the seed photons. Production of electron-positron pairs in the corona limits the minimum possible optical depth and maximum allowed temperature. The emitted spectra consist of the intrinsic IC emission from the hot layer, plus the thermal flux and a reflected component from the cold disk. They are found to be in excellent agreement with present X-ray observations of radio-quiet AGNs.

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