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Title:
The energetics of molecular clouds. III - The S235 molecular cloud
Authors:
Evans, N. J., II; Blair, G. N.
Publication:
Astrophysical Journal, Part 1, vol. 246, June 1, 1981, p. 394-408. Research supported by the Research Corp. (ApJ Homepage)
Publication Date:
06/1981
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
GAS TEMPERATURE, INTERSTELLAR GAS, MOLECULAR CLOUDS, NEAR INFRARED RADIATION, STELLAR EVOLUTION, ABUNDANCE, COSMIC DUST, EMISSION SPECTRA, GAS DENSITY, H II REGIONS, INFRARED ASTRONOMY, INTERSTELLAR MASERS, MASS, SIZE DETERMINATION
Comment:
A&AA ID. AAA029.131.228
DOI:
10.1086/158937
Bibliographic Code:
1981ApJ...246..394E

Abstract

The molecular cloud associated with the S235 H II region has been studied by means of molecular lines and near-infrared observations. The cloud consists of two components, one of which partly surrounds the S235 H II region. The other component contains a dense, hot region of active star formation, marked by self-reversed CO profiles, compact H II regions, masers, and infrared sources. From the molecular line data, the size and mass of the two components are estimated to be 6-8 pc and 3000-4000 solar masses. More detailed studies near the region of active star formation yield estimates of density (approximately 200,000-500,000/cu cm) and the abundances of H2CO, HCO(+), HCN, and (C-13)O. Analysis of the energetics suggests that the cloud is heated by the exciting star of S235 and by the exciting stars of the compact H II regions. Assuming that the gas is heated by collisions with warm dust grains, the far-infrared luminosity has been predicted. The observations of far-infrared emission are in reasonable agreement with predictions.

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