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What is the essential physics of mass loss from late-type stars?A review is given of the data concerning mass loss from late-type stars. The major classes of mass-loss mechanisms (thermally-driven winds, radiatively-driven winds, and wave-driven winds) are discussed, and the empirical mass-loss rates and other data are compared with theoretical predictions for any of these mechanisms acting alone. It is likely that several mechanisms act together to produce the large mass-loss rates in the Mira and nonpulsating M supergiants. Studies of the solar atmosphere suggest that thermal bifurcation driven by molecular condensation instabilities may play a critical role in cooling the atmospheres of luminous cool stars and forming siicate dust. It is possible that several metastable modes of atmospheric structure may exist for a given set of stellar parameters.
Document ID
19880041232
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Linsky, Jeffrey L.
(Joint Institute for Laboratory Astrophysics Boulder, CO, United States)
Date Acquired
August 13, 2013
Publication Date
January 1, 1987
Subject Category
Astrophysics
Meeting Information
Meeting: Circumstellar matter
Location: Heidelberg
Country: Germany
Start Date: June 23, 1986
End Date: June 27, 1986
Sponsors: IAU and DFG
Accession Number
88A28459
Funding Number(s)
CONTRACT_GRANT: NGL-06-003-057
CONTRACT_GRANT: NAG5-82
Distribution Limits
Public
Copyright
Other

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