The dynamical oscillation and propulsion of magnetic fields in the convective zone of a star. I - General considerations

Details The dynamical oscillation and propulsion of magnetic fields in the convective zone of a star. I - General considerations The dynamical oscillation and propulsion of magnetic fields in the convective zone of a star. I - General considerations

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...312..868p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 312, Jan. 15, 1987, p. 868-879.

Physics

72

Convective Heat Transfer, Magnetohydrodynamic Turbulence, Solar Physics, Stellar Activity, Stellar Magnetic Fields, Stellar Oscillations, Magnetic Flux, Stellar Spectrophotometry, Sunspots

Scientific paper

Observations of the sun show that the magnetic flux of the large activity complexes emerges in localized sites in brief bursts at intervals of many days or a few weeks. The quantity of flux arriving at the surface suggests that the mean aximuthal field of the sun in the lower convective zone is not less than 3000 G and may perhaps be considerably more. Such a field inhibits the convective transport of heat. Hence there is a cool shadow on the upper side of the field, and that cool shadow presses downward so hard as to suppress the magnetic buoyancy, forcing the field to remain in the lower convective zone. The accumulation of heat below the field forces intruding fingers of gas up through the field, forming thermal plumes extending up to the visible surface. It is suggested that the process is intermittent, providing a thermal relaxation oscillation with a period of the order of one week. The activity complexes observed at the surface are the consequence of these eruptions of fluid and entrained field from the lower convective zone.

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