The Properties of Compressible MHD Turbulence in Molecular Clouds

Details The Properties of Compressible MHD Turbulence in Molecular Clouds The Properties of Compressible MHD Turbulence in Molecular Clouds

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apr.j2003s&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Present-day star formation in our Galaxy is observed to take place in cold molecular clouds, which appear to be in a state of highly compressible MHD turbulence. Numerical MHD simulations have revealed many important properties of this turbulence. For example, the decay rate of supersonic MHD turbulence is large, indicating it cannot support clouds against gravitational collapse for very long. Moreover, the statisitics of the density, velocity, and magnetic field fluctuations in self-gravitating MHD turbulence are very suggestive of the observed properties of cold clouds. These and other results from direct MHD simulations of the internal dynamics of molecular clouds will be described.

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