Collisional and radiative excitation of SiO masers

Details Collisional and radiative excitation of SiO masers Collisional and radiative excitation of SiO masers

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...102...65b&link_type=abstract

Astronomy and Astrophysics, vol. 102, no. 1, Sept. 1981, p. 65-72.

Astronomy and Astrophysics

Astrophysics

54

Astrophysics, Interstellar Masers, Pumping, Silicon Oxides, Stellar Atmospheres, Astronomical Models, Molecular Collisions, Photons, Radiative Transfer, Stellar Envelopes

Scientific paper

Multilevel calculations are performed to analyze the collisional and radiative pumping of SiO masers. Collisional excitation is recognized as a possible pumping mechanism; a radiative pumping model, in which SiO is located in the inner circumstellar envelope, is then proposed. Unlike the model of Kwan and Scoville (1974), the inversion in a v state is achieved by a direct population transfer from the v-1 state via the absorption of stellar 8 micron photons, followed by an optically thick radiative decay back to v-1. This mechanism is based on the angular dependence of the opacity, which favors the penetration of stellar IR photons into the maser regions. The direction of the maximum amplification is parallel to the star boundaries, and the strongest maser spikes are centered close to the stellar velocity. A comparison of numerical results and observations strongly supports the model.

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