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Mass transfer between binary starsThe transfer of mass from one component of a binary system to another by mass ejection is analyzed through a stellar wind mechanism, using a model which integrates the equations of motion, including the energy equation, with an initial static atmosphere and various temperature fluctuations imposed at the base of the star's corona. The model is applied to several situations and the energy flow is calculated along the line of centers between the two binary components, in the rotating frame of the system, thereby incorporating the centrifugal force. It is shown that relatively small disturbances in the lower chromosphere or photosphere can produce mass loss through a stellar wind mechanism, due to the amplification of the disturbance propagating into the thinner atmosphere. Since there are many possible sources of the disturbance, the model can be used to explain many mass ejection phenomena.
Document ID
19800069585
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Modisette, J. L.
(Houston Baptist University Houston, Tex., United States)
Kondo, Y.
(NASA Goddard Space Flight Center Greenbelt, Md., United States)
Date Acquired
August 10, 2013
Publication Date
January 1, 1980
Subject Category
Astrophysics
Meeting Information
Meeting: Close binary stars: Observations and interpretation
Location: Toronto
Country: Canada
Start Date: August 7, 1979
End Date: August 10, 1979
Accession Number
80A53755
Distribution Limits
Public
Copyright
Other

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