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Thermal instability and energy relations in the convective envelopes of slowly rotating starsThe nonstationary convection that arises due to thermal instability in the envelopes of lower Main Sequence stars (and the sun in particular) is investigated. The convection that arises in the envelopes as a result of thermal instability is of nonstationary turbulent nature. It is shown that construction of a consistent model of the zones of turbulent convection in the stars requires the use of the complete heat flux equation with consideration of the terms that appear because of turbulence. Expressions for these additional terms in terms of averaged characteristics of the motion and eddy viscosity coefficients are derived on the basis of the Prandtl-Wasiutinsky theory.
Document ID
19750005646
Acquisition Source
Legacy CDMS
Document Type
Other
Authors
Yavorskaya, I. M.
(Scripta Publishing Corp. Washington, DC, United States)
Date Acquired
August 8, 2013
Publication Date
November 1, 1974
Publication Information
Publication: Interplanet. Medium and Phys. of the Magnetosphere (NASA-TT-F-784)
Subject Category
Astronomy
Accession Number
75N13718
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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