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Astron. Astrophys. 357, 1123-1132 (2000)

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A note on hydrodynamic viscosity and selfgravitation in accretion disks

W.J. Duschl  *  1,3, P.A. Strittmatter  **  2,3 and P.L. Biermann ***  3

1 Institut für Theoretische Astrophysik, Tiergartenstrasse 15, 69121 Heidelberg, Germany
2 The University of Arizona, Steward Observatory, Tucson, AZ 85721, USA
3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

Received 2 August 1999 / Accepted 3 April 2000

Abstract

We propose a generalized accretion disk viscosity prescription based on hydrodynamically driven turbulence at the critical effective Reynolds number. This approach is consistent with recent re-analysis by Richard & Zahn (1999) of experimental results on turbulent Couette-Taylor flows. This new [FORMULA]-viscosity formulation is applied to both selfgravitating and non-selfgravitating disks and is shown to yield the standard [FORMULA]-disk prescription in the case of shock dissipation limited, non-selfgravitating disks. A specific case of fully selfgravitating [FORMULA]-disks is analyzed. We suggest that such disks may explain the observed spectra of protoplanetary disks and yield a natural explanation for the radial motions inferred from the observed metallicity gradients in disk galaxies. The [FORMULA]-mechanism may also account for the rapid mass transport required to power ultra luminous infrared galaxies.

Key words: accretion, accretion disks – hydrodynamics – turbulence – stars: pre-main sequence – Galaxy: evolution – galaxies: evolution

* wjd@ita.uni-heidelberg.de
** pstrittmatter@as.arizona.edu
*** p165bie@mpifr-bonn.mpg.de

Send offprint requests to: W.J. Duschl, Institut für Theoretische Astrophysik, Tiergartenstrasse 15, 69121 Heidelberg, Germany

Correspondence to: W.J. Duschl, Institut für Theoretische Astrophysik, Tiergartenstrasse 15, 69121 Heidelberg, Germany (wjd@ita.uni-heidelberg.de)

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© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000
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