Non-Linear Evolution of Self-Gravitational MHD Instabilities in Rotating Disks

Details Non-Linear Evolution of Self-Gravitational MHD Instabilities in Rotating Disks Non-Linear Evolution of Self-Gravitational MHD Instabilities in Rotating Disks

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc...40c&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Physics

Scientific paper

We carried out linear analysis and non-linear 3D simulations of self-gravitational magnetohydrodynamics of gas layer in a local co-rotating coordinates. We studied the evolution of Parker-Jeans instability in several cases which are different in factors such as rotational speed, magnetic field, external pressure, external gravitational force, and directions of perturbations. We found that the growth rate of the instabilities and the shape of the dense blobs aggregated in the nonlinear stage sensitively depend on these factors. This study provides us hints on how interstellar/intergalactic gas aggregates to form dense blobs/filaments, which correspond to molecular clouds, under the circumstance of rotation and magnetic field.

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