Other
Scientific paper
Jun 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mmsai..55..215g&link_type=abstract
(European Physical Society, Ministero della Pubblica Istruzione, and Universita di Catania, EPS Study Conference on Oscillations
Other
27
Plasma Frequencies, Stellar Magnetic Fields, Stellar Oscillations, Stellar Rotation, Magnetic Flux, Solar Interior, Solar Rotation
Scientific paper
A formalism to calculate rotational and magnetic splitting of otherwise degenerate high-order oscillation p modes of low degree is outlined. For the purposes of illustration, attention is restricted to axisymmetric toroidal magnetic fields, with axes of symmetry that are permitted to be different from the rotation axis. It is found that advection is the most important contributor to rotational splitting; in general, magnetic perturbations add to the complexity of the frequency spectrum when the oscillations are viewed from an inertial frame. The effect of a field whose axis lies close to the sun's equatorial plane is briefly considered. It is found that such a field is not able to split five-minute dipole modes into observable triplets.
Gough Douglas O.
Taylor Patrick
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