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Modeling Line Emission from Disk Winds

Published online by Cambridge University Press:  03 June 2010

Patrick B. Hall  and
Laura S. Chajet
Patrick B. Hall
Affiliation:
Department of Physics & Astronomy, York University, Toronto, Ontario, Canada Email: phall@yorku.ca, lchajet@yorku.ca
Laura S. Chajet
Affiliation:
Department of Physics & Astronomy, York University, Toronto, Ontario, Canada Email: phall@yorku.ca, lchajet@yorku.ca
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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).

Keywords

galaxies: activequasars: generalquasars: emission lines
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S267: Co-Evolution of Central Black Holes and Galaxies , August 2009 , pp. 398
Copyright
Copyright © International Astronomical Union 2010

References

Murray, N. & Chiang, J. 1997, ApJ, 474, 91CrossRefGoogle Scholar