Disk structure in protostellar H2O maser sources

Details Disk structure in protostellar H2O maser sources Disk structure in protostellar H2O maser sources

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229..593e&link_type=abstract

Astrophysical Journal, Part 1, vol. 229, Apr. 15, 1979, p. 593-603.

Astronomy and Astrophysics

Astronomy

55

Interstellar Masers, Protostars, Stellar Models, Stellar Structure, Stellar Winds, Water Masers, Infrared Astronomy, Kelvin-Helmholtz Instability, Kepler Laws, Stellar Atmospheres, Stellar Envelopes, Stellar Evolution, Stellar Radiation

Scientific paper

Protostellar maser sources are modeled as orbiting gaseous disks surrounding massive windy stars. According to the model, parts of the disk may be H2O masers. The high-velocity features seen in several H2O sources may be due to the material ejected from the inner regions of the disk by pressure from the wind. Radial intervals in which the gas density is suitable for a maser determine the velocity and distance range of these features. Maser spot size, the temperatures and densities in the maser region, and the duration of the maser phase can all be accounted for through reference to the model.

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