Physics
Scientific paper
Jun 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mmsai..55..273r&link_type=abstract
(European Physical Society, Ministero della Pubblica Istruzione, and Universita di Catania, EPS Study Conference on Oscillations
Physics
2
Solar Interior, Solar Neutrinos, Solar Rotation, Spin Dynamics, Turbulent Diffusion, Angular Momentum, Angular Velocity, Momentum Transfer, Solar Physics, Stellar Models
Scientific paper
The sun is losing angular momentum through the mass loss in the solar wind and must therefore have spun down from higher velocities during its lifetime. This angular momentum loss will produce differential rotation in the solar interior unless magnetic fields are retained in the interior and are able to transport angular momentum by magnetic stresses. In this paper the author assumes magnetic fields are not effective in the bulk of the interior and shows that when the radial angular velocity reaches a critical value, baroclynic overstability sets in. This instability drives the inward diffusion of 1H. The increase of the central 1H abundance will lead to a reduction of the detectable neutrino flux.
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