Convective stability in magnetic stars

Details Convective stability in magnetic stars Convective stability in magnetic stars

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..71..111s&link_type=abstract

Astrophysics and Space Science, vol. 71, no. 1, Aug. 1980, p. 111-121.

Mathematics

Convection, Dynamic Stability, Magnetic Stars, Oscillations, Axisymmetric Bodies, Potential Energy, Stellar Magnetic Fields, Taylor Instability, Transformations (Mathematics)

Scientific paper

Dynamical stability of a static axisymmetrical magnetic star with respect to high-order modes of oscillation is investigated by means of the energy method, neglecting the Eulerian perturbation of gravity. The magnetic field is assumed to be continuous across the surface of the star and its first-order spatial derivatives, but it may have both toroidal and poloidal components. The second variation of the potential energy is written in a way which, in the case of a purely toroidal field, and for axisymmetrical and non-axisymmetrical modes, yields Tayler's local stability criteria which are necessary and sufficient conditions for convective stability, and in the case of a general field yields a single local stability criterion, which is a sufficient condition for convective stability.

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