The mechanical equilibrium of interstellar clouds - Scaling relations for gas density, line width, and magnetic field strength

Details The mechanical equilibrium of interstellar clouds - Scaling relations for gas density, line width, and magnetic field strength The mechanical equilibrium of interstellar clouds - Scaling relations for gas density, line width, and magnetic field strength

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..299f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 1, 1988, p. 299-303.

Astronomy and Astrophysics

Astrophysics

28

Gas Density, Interstellar Magnetic Fields, Molecular Clouds, Spectral Line Width, Field Strength, H I Regions, Nebulae, Turbulence

Scientific paper

A virial model is developed for a hierarchy of self-gravitating, turbulent magnetic clouds in pressure equilibrium with their surroundings. A complete set of scaling relations for gas volume density, column density, internal velocity dispersion, and magnetic field strength is derived and compared with the observed relations. Pressure-confined clouds having negligible self-gravity are modeled, and a set of scaling relations for the change in velocity and for the magnetic field strength are obtained. These results are compared with observations of velocity line width and magnetic field strength in diffuse H I clouds and in pressure-confined molecular clouds.

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