Modeling Line Emission from Disk Winds

Details Modeling Line Emission from Disk Winds Modeling Line Emission from Disk Winds

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010iaus..267..398h&link_type=abstract

Co-Evolution of Central Black Holes and Galaxies, Proceedings of the International Astronomical Union, IAU Symposium, Volume 267

Astronomy and Astrophysics

Astronomy

3

Galaxies: Active, Quasars: General, Quasars: Emission Lines

Scientific paper

Murray & Chiang (1997) developed a model wherein broad emission lines come from the optically thick base of a rotating, outwardly accelerating wind at the surface of an accretion disk. Photons preferentially escape radially in such a wind, explaining why broad emission lines are usually single-peaked. Less well understood are the observed shifts of emission-line peaks (from 1000 km s-1 redshifted to 2500 km s-1 blueshifted in C iv, with an average 800 km s-1 blueshift).

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