Density Waves and WARPS Generated by Tidal Perturbation of a Gaseous Disk

Details Density Waves and WARPS Generated by Tidal Perturbation of a Gaseous Disk Density Waves and WARPS Generated by Tidal Perturbation of a Gaseous Disk

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995nyasa.773..261p&link_type=abstract

Waves in Astrophysics, vol. Volume 773, p. 261-276

Astronomy and Astrophysics

Astrophysics

3

Tides, Accretion Disks, Binary Stars, Rotating Disks, Planar Structures, Stellar Systems, Stellar Orbits, Circular Orbits, Thickness, Rigid Structures, Inviscid Flow

Scientific paper

Recently much progress has been made in our knowledge of pre-main sequence binary and multiple stars that apparently form the majority of young stellar systems. Disk-companion interactions leading to tidal truncation and sculpting of the disk have previously been studied in the context of close binary systems and the early solar system. In these cases, circular or near-circular coplanar orbits were assumed for the binary. In this paper we consider an inviscid disk undergoing tidal interaction as a result of a perturber flying by on a coplanar parabolic orbit. A sequence of such encounters also approximates the situation appropriate to a companion in a highly eccentric orbit. We extend previous calculations to consider the case when the perturbing mass is one-tenth of the central mass. Later we consider the disk response when the perturber's orbit is circular, not coplanar. We consider the zero-frequency perturbation that provides a net torque on the disk and that would cause it, if rigid, to precess as a rigid body. We evaluate the linear response of a disk with varying thickness when the perturbing and central mass are equal. If the binary separation is great enough, the response is found to be similar to that of a rigid body.

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