Magnetic fields and non-uniform rotation in stellar radiative zones

Details Magnetic fields and non-uniform rotation in stellar radiative zones Magnetic fields and non-uniform rotation in stellar radiative zones

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.226..123m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 226, May 1, 1987, p. 123-135.

Astronomy and Astrophysics

Astronomy

115

Dynamo Theory, Stellar Magnetic Fields, Stellar Rotation, Angular Momentum, Conductivity, Magnetic Effects, Momentum Transfer, Stellar Radiation

Scientific paper

This paper examines the effects of dynamical and resistive instabilities on magnetic redistribution of angular momentum within a star. It is tentatively concluded that if significant differential rotation survives in a stably stratified radiative zone over a stellar evolution time, then the poloidal field, Bp, cannot exceed an upper limit of order 3×10-2G and is probably less than 10-3G. In the radiative core of the Sun Bp is estimated to be at least of order 5×10-2G and probably 100 G or more. Values greater than 0.1 G cannot easily be reconciled with the rotational shear inferred from frequency splitting of solar oscillations.

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