Mixing motions in the sun and solar-type stars

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Solar Rotation, Stellar Magnetic Fields, Stellar Models, Stellar Motions, Sun, Adiabatic Conditions, Centrifugal Force, Convective Flow, Magnetic Effects, Solar Interior, Stellar Rotation

Scientific paper

Consideration is given to some of the consequences of adiabatic, dynamically driven motions within the radiative inner region of the sun and solar-type stars for which it is assumed that an oblique magnetic field is trapped below the convection zone. The internal motions derive both from centrifugal and magnetic forces, and their behavior over the lifetime of a solar-type star is discussed. Following Mestel (1975), it is assumed that stars of approximately one solar mass have a magnetic field that is contained by the outer convection zones of solar-type stars. It is contended that if such a field exists in the interior of the sun and other solar-type stars, then coupled with the possibility of a rapidly rotating core there is a possible mechanism for diffusive-type motions that could influence solar models. In addition, it is shown that if the nutation frequency of an oblique magnetic rotator corresponds to the solar cycle, then the magnetic field will need to be of the order of 10 to the 7th G.

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