Theoretical emission line profiles in the spectra of active galactic nuclei

Details Theoretical emission line profiles in the spectra of active galactic nuclei Theoretical emission line profiles in the spectra of active galactic nuclei

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988baicz..39..345h&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 39, no. 6, Dec. 1988, p. 345-354.

Astronomy and Astrophysics

Astronomy

4

Active Galactic Nuclei, Astronomical Spectroscopy, Emission Spectra, Gas Flow, Line Spectra, Compton Effect, Interstellar Gas, Stellar Winds

Scientific paper

The gas outflow from an active galaxy nucleus is modelled by the stellar wind driven by short wavelength radiation of the central source. The emission clouds are assumed to arise in this gas due to its thermal bistability. The motion of emission clouds is calculated in the inner zone of the nucleus envelope. The radiative pressure, friction due to the relative motion of the cloud with respect to the confining gas and the gravitation of the central body are taken into account. The line profiles of the hydrogen lines radiated by the clouds are computed for both cases of the narrow stream and their motion inside a wide cone.

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