A model for OH masers in star-forming regions

Details A model for OH masers in star-forming regions A model for OH masers in star-forming regions

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.252...30g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 252, Sept. 1, 1991, p. 30-48.

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Astronomical Models, Hydroxyl Emission, Interstellar Masers, Star Formation, Computational Astrophysics, Cosmic Dust, H Ii Regions, Infrared Radiation, Molecular Excitation, Spectral Emission

Scientific paper

A new model of the OH maser environment in star-forming regions is described, and the model's predictions are compared with observational data. The status of OH maser observations is reviewed, and the ingredients which such a model requires are outlined. Steady-state rate equations are derived and solved using the large velocity gradient approximation for 48 OH hyperfine-level populations for a broad range of physical conditions. The present predictions are compared with VLA observations by Gaume and Mutel (1987) for ground-state masing action. It is shown that the effects of line overlap in accelerating outflows (or inflows) are crucial in order to reproduce the most important qualitative features of these data, e.g., the preponderance of 1665-MHz emission. Excited-state masers are considered with special reference to observed correlations between excited- and ground-state maser action. It is inferred that the observational properties of OH masers are consistent with a moderately warm and dense environment sustaining bulk flows of material.

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