CO radio-line profiles in cold interstellar clouds

Details CO radio-line profiles in cold interstellar clouds CO radio-line profiles in cold interstellar clouds

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985azh....62..860z&link_type=abstract

(Astronomicheskii Zhurnal, vol. 62, Sept.-Oct. 1985, p. 860-870) Soviet Astronomy (ISSN 0038-5301), vol. 29, Sept.-Oct. 1985, p.

Astronomy and Astrophysics

Astronomy

4

Carbon Monoxide, Interstellar Gas, Line Spectra, Molecular Clouds, Radio Astronomy, Monte Carlo Method, Radial Distribution, Radial Velocity

Scientific paper

A discussion of how properly to interpret the self-reversed CO radio-line profiles observed in dark clouds indicates for the first time that such profiles can develop in a collapsing, microturbulent model cloud whose excitation temperature rises outward from the center. Monte Carlo calculations yield sets of profiles for a spherically symmetric cloud with a quadratic density distribution and several laws for the radial dependence of the contraction velocity. The computed profiles are compared against observations of the dust cloud L673.

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