The Fate of an Unstable Mode

Details The Fate of an Unstable Mode The Fate of an Unstable Mode

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aspc..160..132l&link_type=abstract

Astrophysical Discs - An EC Summer School, Astronomical Society of the Pacific, Conference series Vol #160, Edited by J. A. Sell

Astronomy and Astrophysics

Astrophysics

Scientific paper

This contribution draws from our efforts to seek a better understanding of the behaviour of self-gravitating discs. Our specific approach consists of performing a detailed analysis of a simplified model disc which is susceptible to the growth of a two-armed spiral. We first perform a numerical simulation of this disc. The outcome of the simulation is then used to motivate both a linear and a nonlinear perturbative analysis of the hydrodynamic governing equations. We see evidence that the dramatic early phase of mass and angular momentum transport in the disc can be explained by a second-order nonlinear process involving self-interaction of the dominant (m=2) linear mode. This rapid transport may be instrumental in allowing unstable discs to re-adjust their structure and avoid fragmentation.

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