High velocity molecular emission in Orion - A case for stellar winds

Details High velocity molecular emission in Orion - A case for stellar winds High velocity molecular emission in Orion - A case for stellar winds

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...251...88k&link_type=abstract

Astrophysical Journal, Part 1, vol. 251, Dec. 1, 1981, p. 88-102. NASA-supported research

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43

Emission Spectra, Interstellar Masers, Molecular Spectra, Orion Nebula, Stellar Winds, Water Masers, Infrared Spectra, Line Shape, Main Sequence Stars, Molecular Gases, Plasma-Particle Interactions, Shock Waves

Scientific paper

On the basis of data from the literature and observations of both a variety of molecules in the high-velocity source of the Orion molecular cloud and high-velocity emissions in other molecular clouds, it is proposed that the high-velocity source consists of clumps of dense molecular gas which are accelerated by the high-velocity stellar wind of a pre-main sequence star. Some of the H2O maser emissions, and the H2 and Herbig-Haro-type emissions, are attributed to shocks associated with the breakup of the protostellar cocoon.

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