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An Accretion Disk Model for the Innermost 200PC of the Galaxy

Published online by Cambridge University Press:  12 April 2016

W.J. Duschl ,
S.v. Linden  and
P.L. Biermann
W.J. Duschl
Affiliation:
Institut für Theoretische Astrophysik, Universität Heidelberg, Im Neuenheimer Feld 561, W-6900 Heidelberg, Germany
S.v. Linden
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, W-5300 Bonn, Germany
P.L. Biermann
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, W-5300 Bonn, Germany

Abstract

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We demonstrate that it is possible to understand observed radial velocities of molecular clouds close to the Galactic Center as being due to motion of this material in an accretion disk. Our models indicate a stationary disk with a radial mass flow rate of 10-1.8 Mʘ/yr with a viscosity of 1.9 · 103 pc km/s at 100 pc from the Galactic Center and a radial dependence of it, that goes approximately like the square root of the radius from the Galactic Center.

Type
3. Astronomical Results and Prospects
Information
International Astronomical Union Colloquium , Volume 140: Astronomy with Millimeter and Submillimeter Wave Interferometry , 1994 , pp. 174 - 175
Copyright
Copyright © Astronomical Society of the Pacific 1994