Disk Winds and Quasar Broad Emission Lines
As matter slowly spirals into a supermassive black hole at the
center of a massive galaxy, it can produce the light we call
a quasar. The matter forms a thin accretion disk which heats
up and gives off blackbody radiation at a range of temperatures.
Quasars also show emission lines from ionized gas moving at
speeds of thousands of km/s, usually with an overall blueshift.
This line-emitting gas is likely to arise in an optically thick,
outwardly accelerating wind at the surface of the accretion disk;
such winds are likely needed to explain the single-peaked emission
lines of quasars. I'll present preliminary results of new models
of such winds which aim to reproduce the observed velocity shifts,
line shapes, and aspects of the line width distribution in quasars.
|Date: ||Jeudi, le 12 mars 2009|
|Lieu: ||Université de Montréal|
| ||Pavillon Roger-Gaudry, Local D-460|
|Contact: ||Pierre Bergeron|