The Molecular Cloud Associated with the HII Region RCW:34

Details The Molecular Cloud Associated with the HII Region RCW:34 The Molecular Cloud Associated with the HII Region RCW:34

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...275..573p&link_type=abstract

Astronomy and Astrophysics, Vol.275, NO.2/AUG(II), P. 573, 1993

Astronomy and Astrophysics

Astrophysics

4

Interstellar Medium: H Ii Regions: Rcw 34, Molecules: Co, Cs, Hcn, Abundances: 13C, 18O, Molecular Cloud, Radiative Transfer

Scientific paper

We present millimetric multi-line observations of the molecular cloud associated with the H II region RCW 34. We believe we are able to present a coherent description of the cloud: a molecular bar on top of the H II region is divided into three elements: a dense, heated part situated in the post-shock trail, a cold, less dense part besides, left unperturbed and a diffuse component either in front of the dense parts or possibly mixed with them if the dense parts are clumpy. This diffuse component has a density of a few hundreds per cm-3, a temperature in the range 30-60 K and its opacity in 12CO is close to or less than unity. We show that this diffuse component, the existence of which is controversial, is the best explanation to the large 12CO (J: 1 → 0)/(J: 2 → 1) ratio we have observed. A simple-minded model is presented to approach its properties. The cloud is on top and partly in front of the H II region and can explain the 4.2 mag of visual extinction measured by one of us (Heydari-Malayeri 1988). The very high velocity flow detected in Hα by Heydari-Malayeri has no counterpart in radio but could be a direct visualisation of the so-called "Champagne effect" (Tonorio-Tagle 1979).

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