Theory of astrophysical SiO masers

Details Theory of astrophysical SiO masers Theory of astrophysical SiO masers

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...284..751l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 284, Sept. 15, 1984, p. 751-768.

Statistics

Computation

59

Interstellar Masers, Red Giant Stars, Stellar Envelopes, Stellar Winds, Computational Astrophysics, Late Stars, Radiative Transfer, Silicon Oxides, Sobolev Space, Stellar Models, Stellar Spectra, Vibrational Spectra

Scientific paper

Circumstellar masing in the vibrationally excited states of SiO has been observed in many sources and is particularly common in oxygen-rich, late-type giants. Model calculations for SiO maser emission in a smooth stellar wind are presented for a variety of system parameters appropriate for a late-type giant. The Sobolev approximation is used to describe the radiative transfer. Analogous calculations have been performed by previous investigators, but improvements in the calculational methods together with current information about the input physical data lead to conclusions that are qualitatively different. It is found that models employing a smooth wind yield less maser power than is reported from the neighborhood of late-type giants. The models do, however, exhibit many of the other features of the SiO masers. The accuracy of the Solobev approximation is examined by numerically integrating the exact equations of radiative transfer. It is found to be quite inaccurate for certain plausible physical conditions in the outflowing wind, and tends to overestimate the maser power.

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