Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...20719701m&link_type=abstract
American Astronomical Society Meeting 207, #197.01; Bulletin of the American Astronomical Society, Vol. 37, p.1495
Astronomy and Astrophysics
Astronomy
Scientific paper
Two-thirds of type I AGN exhibit outflows of ionized absorbing gas. The location, origin and dynamics of these ionized outflows are poorly understood. I will present the results from the first uniform analysis of the ionized absorbers in a small sample of type I AGN observed with the gratings on board the Chandra X-ray telescope.
Our results for the hot outflows from AGN agree well with the model of Krolik & Kriss of photoionized evaporation of a dusty torus. The mass carried by the hot outflows seems very high; it is comparable with the expected accretion rate onto the black hole, as predicted by Krolik & Kriss. The measured distance of the hot gas from the continuum source is also consistent with the Krolik & Kriss model, if the electron density in the hot gas is ≤ 108 {cm}-3. The Elvis model of hot outflows from AGN, namely a vertical disk wind, blown outwards in a funnel-shaped outflow, is much more strongly constrained by our work. The parameter space of the hot outflows is relatively small, suggesting both a narrow angle of AGN inclination and a narrow range of parameters for the disk wind. The Elvis model predicts that the Fe K line is produced in the hot outflow and not in the accretion disk. However, we find that there is no correlation between the equivalent width of the Fe K line and the column density of gas in the hot outflow.
One new result was only obtainable from a uniform analysis of a sample of AGN. We find, intriguingly, that the larger the rate of growth of the AGN central black hole, apparently the smaller the velocity of the hot outflow.
We gratefully acknowledge support from NSF grant AST0205990 & from Coastal Carolina University.
McKernan Barry
Reynolds Chris S.
Yaqoob Tahir
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