Shells, outflows and star formation in the giant molecular cloud Monoceros R2

Details Shells, outflows and star formation in the giant molecular cloud Monoceros R2 Shells, outflows and star formation in the giant molecular cloud Monoceros R2

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992phdt.........2x&link_type=abstract

Ph.D. Thesis Massachusetts Univ., Boston.

Astronomy and Astrophysics

Astronomy

7

Molecular Clouds, Point Sources, Reflection Nebulae, Star Formation, Dust, Emission Spectra, Infrared Astronomy Satellite, O Stars, Red Shift, Stellar Winds

Scientific paper

To improve our understanding about giant molecular clouds (GMC) associated with R-associations, a CO-12 J = 1-0 map of 167,000 spectra with 45 inch resolution and 25 inch spacing, a CO-13 J = 1-0 map of approximately 40,000 spectra with 1.5 foot resolution and 1 foot spacing, IRAS BIGMAP images, and maps of high density molecular tracers for the dense cores are obtained for the GMC Monoceros R2 (D = 830 plus or minus 50 pc). These data reveal that the large-scale structure of Mon R2 is dominated by an expanding bubble shell (approximately 30 pc) with front side moving towards us at a radial velocity of approximately 4-5 km/s. Distortions of this shell are obvious, suggesting of the inhomogeneity of the cloud before the formation of the bubble. There is no evidence for red-shifted shell at the far side of the bubble. There are at least two generations of star formation in Mon R2. The older generation of stars with an age of 6-10 x 106 years are represented mostly by reflection nebulae. The younger generation of stars with an age of approximately 105 years are represented mostly by IRAS point sources. It is proposed that the large-scale expanding bubble shell is the result of combined effects of ionizing flux and stellar winds originating from the older generation of young stellar objects, but perhaps dominated by O type stars which either are obscured or left main sequence. It is suggested that the formation of the younger generation of stars has been triggered by the older generation of stars. The main and the GGD12-15 cores are located on the large-scale expanding shell, and their harboring both generations of stars can be explained were the cores preexisting clumps. Our CO data reveal an eggplant-shaped bipolar outflow shell, whose shape can be satisfactorily modeled with radially directed stellar winds sweeping up ambient material with momentum conservation. An inversion method is implemented for analyzing dust emission spectra at FIR wavelengths in terms of a continuous dust temperature distribution, and was applied to IRAS BIGMAP images of Mon R2. Computer programs are developed for identifying clumps and determining their properties in molecular emission maps. The results support the reality of size-linewidth and mass-linewidth relations for clumps in individual GMC's.

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