Radiation transport and the kinematics of molecular clouds

Details Radiation transport and the kinematics of molecular clouds Radiation transport and the kinematics of molecular clouds

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...223..147k&link_type=abstract

Astrophysical Journal, Part 1, vol. 223, July 1, 1978, p. 147-160.

Astronomy and Astrophysics

Astrophysics

41

Interstellar Matter, Molecular Spectra, Nebulae, Radiative Transfer, Astronomical Models, Carbon Monoxide, Kinematics, Millimeter Waves, Spectral Line Width

Scientific paper

The large widths of millimeter molecular lines have been interpreted as being due to either systematic motion or local turbulence in molecular clouds. This paper evaluates the merits of each interpretation by comparing line profiles produced in either a systematic motion or a turbulent motion under the same conditions of temperature and density with the stipulation that both temperature and density decrease with increasing distance from a central point. Molecular-line observations of the M17 SW region and the Kleinmann-Low (KL) nebula are analyzed, particularly with respect to various CO and CS lines. It is found that the observations of M17 SW are best explained by a model in which turbulence dominates the central part of the molecular region but collapse prevails in the outer part, while the observations of the KL nebula can be equally well explained by either of two models. The first model postulates that KL is at the front face of the molecular cloud and turbulence gives rise to the line broadening; the second places KL deep within the molecular cloud and attributes only the CO line widths to systematic motion about the nebula.

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