Hydrostatic models of molecular clouds. II - Steady state models of spherical clouds

Details Hydrostatic models of molecular clouds. II - Steady state models of spherical clouds Hydrostatic models of molecular clouds. II - Steady state models of spherical clouds

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...134...87b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 134, no. 1, May 1984, p. 87-98. Research supported by the Stichting Astronomis

Astronomy and Astrophysics

Astrophysics

58

Astronomical Models, Hydrostatics, Interstellar Chemistry, Molecular Clouds, Abundance, Brightness Temperature, Chemical Equilibrium, Chemical Reactions, Cooling, Gas Ionization, Heating, Molecular Spectra, Radio Spectra, Steady State

Scientific paper

Self-gravitating spherical models have been constructed of small molecular clouds without internal heat sources supported by turbulent and thermal pressure, assuming thermal balance and chemical equilibrium and a circulation of matter on a turbulent time scale (so that undepleted gas is returned from the outer layers to the cloud core). In the inner parts of the cloud, the gas is predominantly heated by cosmic ray ionizations and energy dissipation of turbulent motions. The models considered exhibit a definite core-halo structure. If matter in the cloud is circulated at a velocity corresponding to Mach number alpha, the heavy element depletion factor changes from 0.5 at the cloud surface to 0.07 in the core for an alpha value of 1 and 0.009 for alpha of 0.5. It is concluded that the circulation model accounts for the metal depletion factors required to keep from upsetting the low degree of ionization in molecular cloud cores.

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