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2000ApJ...543..686P - Astrophys. J., 543, 686-696 (2000/November-2)
Dynamics of line-driven disk winds in active galactic nuclei.
PROGA D., STONE J.M. and KALLMAN T.R.
Abstract (from CDS):
We find that a disk accreting onto a 108 M☉ black hole at the rate of 1.8 M☉.yr–1 can launch a wind at ∼1016 cm from the central engine. The X-rays from the central object are significantly attenuated by the disk atmosphere so they cannot prevent the local disk radiation from pushing matter away from the disk. However, in the supersonic portion of the flow high above the disk, the X-rays can overionize the gas and decrease the wind terminal velocity. For a reasonable X-ray opacity, e.g., κX=40 g–1.cm2, the disk wind can be accelerated by the central UV radiation to velocities of up to 15,000 km.s–1 at a distance of ∼1017 cm from the central engine. The covering factor of the disk wind is ∼0.2. The wind is unsteady and consists of an opaque, slow vertical flow near the disk that is bounded on the polar side by a high-velocity stream. A typical column density through the fast stream is a few times 1023 cm–2 so the stream is optically thin to the UV radiation. This low column density is precisely why gas can be accelerated to high velocities. The fast stream contributes nearly 100% to the total wind mass-loss rate of 0.5 M☉.yr–1.
Abstract Copyright: ∼
Journal keyword(s): Accretion, Accretion Disks - Galaxies: Active - Hydrodynamics - Instabilities - Methods: Numerical
Simbad objects: 1
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