Self-reversed CO profiles in collapsing molecular clouds

Details Self-reversed CO profiles in collapsing molecular clouds Self-reversed CO profiles in collapsing molecular clouds

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...211..122s&link_type=abstract

Astrophysical Journal, vol. 211, Jan. 1, 1977, pt. 1, p. 122-127. Research supported by the Robert A. Welch Foundation

Astronomy and Astrophysics

Astrophysics

89

Carbon Monoxide, Gravitational Collapse, Interstellar Matter, Line Spectra, Molecular Spectra, Nebulae, Astronomical Models, Astronomical Spectroscopy, Cosmic Dust, Emission Spectra, Spectral Line Width

Scientific paper

Observations of self-reversed CO line profiles in four dense molecular clouds (Mon R2, NGC 1333, W3, and Rho Oph) are discussed, and it is shown that these cases are readily explained by self-absorption in the outer layers of a nonhomologously collapsing cloud. Common features of the four clouds are reviewed, evidence is presented which indicates that the clouds are in a state of collapse rather than expansion, and it is demonstrated that the collapse is most likely nonhomologous with the collapse velocity varying as the inverse square root of cloud radius. CO line profiles are calculated with and without small amounts of turbulent broadening for a spherically symmetric nonhomologous collapsing cloud; these are compared with observed line-of-sight CO and (C-13)O line profiles. The general agreement between the line profiles given by the model with a small amount of turbulence and the observed line profiles is found to be quite good, with all the common features of the observed profiles present in the calculated profiles. An observational test of the model is proposed.

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