SiO isotopes in Orion A

Details SiO isotopes in Orion A SiO isotopes in Orion A

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...100l..30o&link_type=abstract

Astronomy and Astrophysics, vol. 100, no. 2, July 1981, p. L30-L33.

Astronomy and Astrophysics

Astrophysics

41

Interstellar Masers, Interstellar Matter, Isotopes, Maser Outputs, Orion Nebula, Silicon Oxides, Brightness Temperature, Molecular Clouds, Population Inversion

Scientific paper

Time variable features are observed in the Orion (Si-29)O (v = 0, J = 2-1) emission, presumably of maser origin. The corresponding (Si-30)O line shows a very different line shape and could also be influenced by maser effects. No signs of variability are seen in the (Si-28)O (v = 0, J = 2-1) emission, which appears to be partly saturated. The population inversion machanism must be very selective, suggesting influences of IR line overlap and/or opacity effects. A mapping of the (Si-28)O (v = 0, J = 2-1) line reveals three separable emission regions within an area considerably smaller than the 43-arcsec beam. The centroids of the blue- and red-shifted high-velocity flows appear to be displaced approximately 8 arcsec to the NW and approximately 4 arcsec to the NE of the lower velocity shell emission, respectively.

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