Aspects of Self-Gravitating, Magnetized Interstellar Turbulence

Details Aspects of Self-Gravitating, Magnetized Interstellar Turbulence Aspects of Self-Gravitating, Magnetized Interstellar Turbulence

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aps..dpp.gm106g&link_type=abstract

American Physical Society, 41st Annual Meeting of the Division of Plasma Physics, November 15-19, 1999 Seattle, WA, abstract #GM

Physics

Plasma Physics

Scientific paper

I will discuss recent progress in understanding turbulence in the cold interstellar medium; this turbulence is self-gravitating, magnetized (δ v/vA ~ 1), and supersonic (δ v/cs >> 1). It is of great interest to astronomers because the cold interstellar medium is the site of star formation. Aspects of this ``protostellar'' turbulence are likely to play an important role in determining the stellar initial mass spectrum. Progress in this field has been enabled by the development of high-resolution numerical codes that accurately follow a compressible, isothermal fluid in ideal MHD. I will focus on an analysis of the regions around density maxima in a series of new simulations.

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