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Gravitational Instabilities in Circumstellar Disks and the Formation of Binary Companions

Published online by Cambridge University Press:  12 April 2016

Fred C. Adams  and
Willy Benz
Fred C. Adams
Affiliation:
Physics Department, University of Michigan, Ann Arbor, MI 48109, USA
Willy Benz
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA

Abstract

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We review recent work on gravitational instabilities in circumstellar disks and discuss implications for the possibility of forming binary companions within these disks. Linear stability analysis indicates that self-gravitating modes with azimuthal wavenumber m = 1 will grow strongly in star/disk systems with the physical properties observed in astrophysical systems. Smooth particle hydrodynamic simulations indicate that these self-gravitating instabilities (with m = 1 and higher) will grow into the nonlinear regime. In many cases, a spiral arm will collapse into a gravitationally bound “knot” of gas; these knots typically contain 1% of the mass of the disk and travel on elliptical orbits about the central star.

Type
Theoretical Aspects
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 185 - 194
Copyright
Copyright © Astronomical Society of the Pacific 1992

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