The C1/CO/ Ratio in the Molecular Cloud G:34.3+0.2

Details The C1/CO/ Ratio in the Molecular Cloud G:34.3+0.2 The C1/CO/ Ratio in the Molecular Cloud G:34.3+0.2

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.271..649l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 271, NO. 3/DEC1, P. 649, 1994

Astronomy and Astrophysics

Astronomy

21

Scientific paper

A model for the structure of the massive molecular cloud G 34.3+0.2 is derived from extensive observations of carbon monoxide lines, including J= 1-0, J= 2-1, J= 3-2 and J= 6-5 13CO, and J= 2-1 C18O. The model consists of a slowly collapsing turbulent cloud with density constant out to a radius of 0.15 pc, but falling off as R-2 out to 3.25 pc. The CO abundance is constant. Within the framework of the basic cloud structure it is possible to predict line shapes for the 492-GHz 3P1-3P0 C' line, for different assumed radial behaviour of the C i abundance. These are compared with observations. The best fit is found with C ioc from the perimeter of the cloud into r =0.24 pc where A =55. The column-density-averaged [C ii![COi ratio for G 34.3+0.2 is very similar to that for the o Ophiuchi molecular cloud, notwithstanding the very different structures of the two clouds. Models for producing high carbon abundances deep in clouds that may have difficulty in explaining the results include those with external ultraviolet penetration around clumps, or dynamic mixing, or in which the initial [Cj/[OJ ratio is greater than unity. Key words: line: profiles - ISM: abundances - ISM: clouds - ISM: individual: G 34.3+0.2 - ISM: molecules - radio lines: ISM.

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