Other
Scientific paper
Oct 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982nyasa.395..220e&link_type=abstract
(NASA, National Science Foundation, New York Academy of Sciences, et al., Symposium on the Orion Nebula to Honor Henry Draper, N
Other
Interstellar Masers, Late Stars, Orion Nebula, Silicon Oxides, Cosmic Dust, Cosmic Gases, Gas Temperature, Radiation Pressure, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Velocity Distribution
Scientific paper
The concepts developed for SiO masers in late-type stars are discussed in an effort to understand the Orion SiO maser and its apparent uniqueness. A consistent set of parameters is obtained that can explain the SiO maser operation in Orion and, possibly, also provide an explanation for the lack of such action in the other star-formation regions so far observed. The SiO maser emission from Orion is seen as providing a rare opportunity to observe the transition from a chaotic to an ordered velocity field due to radiation pressure on grains that have just formed. The reason that star-forming regions do not generally support SiO maser action may be the need for very high mass-loss rates (approximately 0.001 solar mass/yr) as well as the rather close coincidence of parameters; this leads to the gas being warmer than the dust over a sufficiently large region.
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