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Fine structure line emission from supergiantsWe have detected (O I) 63 micron and (Si II) 35 micron emission from the oxygen-rich, M supergiants alpha Orionis (Betelgeuse), alpha Scorpii (Antares), and alpha Herculis (Rasalgethi). The measured fluxes indicate that the emission originates in dense, warm gas in the inner envelope or transition region where molecules and dust are expected to form and the acceleration of the wind occurs. Mass-loss rates are derived, evidence for time variability is presented, and results for other evolved stars are included.
Document ID
19960003667
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Haas, Michael R.
(NASA Ames Research Center Moffett Field, CA, United States)
Glassgold, Alfred E.
(New York Univ. New York, NY., United States)
Tielens, Alexander G. G. M.
(NASA Ames Research Center Moffett Field, CA, United States)
Date Acquired
September 6, 2013
Publication Date
January 1, 1995
Publication Information
Publication: Astronomical Society of the Pacific, Airborne Astronomy Symposium on the Galactic Ecosystem: From Gas to Stars to Dust, Volume 73
Subject Category
Space Radiation
Accession Number
96N13677
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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