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Rotation in solar-type stars. I - Evolutionary models for the spin-down of the sun
Endal, A. S.; Sofia, S.
AA(Louisiana State University, Baton Rouge, La.), AB(NASA, Goddard Space Flight Center, Laboratory for Planetary Atmospheres, Greenbelt, Md.)
Astrophysical Journal, Part 1, vol. 243, Jan. 15, 1981, p. 625-640. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Main Sequence Stars, Solar Rotation, Stellar Evolution, Stellar Models, Stellar Rotation, Abundance, Angular Momentum, Convective Flow, Radiative Transfer, Solar Wind, Stellar Structure
Bibliographic Code:


Models of rotating, 1 solar mass stars through the pre-main sequence and main sequence stages have been calculated. The calculations begin on the Hayashi track with rapid, rigid-body rotation, with angular momentum removed from the convective envelope to simulate the effect of the solar wind as the models evolve. Interior angular momentum redistribution by circulation flows and rotational instabilities is computed by a diffusion technique. It is found that at the present age of solar evolution, the models employed have internal rotation rates significantly larger than those allowed by measured solar oblateness, suggesting that the effects of circulation currents near the outer boundary of the radiative interior have been underestimated. An important result of this study is the implication that circulation currents produce deep mixing of such minor constituents as He-3 and C-13, perhaps also explaining the observed steady depletion of lithium during the main-sequence stage.

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Database: Astronomy
arXiv e-prints