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Doubly diffusive magnetic buoyancy instability in the solar interiorAn investigation of the buoyancy of diffuse magnetic fields has shown that in the presence of rotation, static equilibrium configurations of the toroidal magnetic field and ambient plasma can exist. In that case, the escape of toroidal magnetic flux from the solar interior may be determined by the growth of instabilities which the equilibrium configuration may be subject to. In connection with the present investigation, it is assumed that in the region of toroidal magnetic flux amplification, the magnetic field has not as yet filamented into flux ropes, and is therefore 'diffuse'. A study is conducted of the MHD stability of an electrically conducting and differentially rotating gas in the presence of a toroidal magnetic field, an external constant gravitational field, and radiance pressure. The full dispersion relation for the magnetic buoyancy problem is developed, and the solutions of the dispersion relation are discussed.
Document ID
19830041839
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Schmitt, J. H. M. M.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Rosner, R.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 11, 2013
Publication Date
February 15, 1983
Publication Information
Publication: Astrophysical Journal
Subject Category
Solar Physics
Accession Number
83A23057
Funding Number(s)
CONTRACT_GRANT: NAGW-79
Distribution Limits
Public
Copyright
Other

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