Magnetic fields in the overshoot zone: The great escape

Details Magnetic fields in the overshoot zone: The great escape Magnetic fields in the overshoot zone: The great escape

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987nascp2483..101c&link_type=abstract

In NASA-Goddard Space Flight Center, Theoretical Problems in High Resolution Solar Physics, 2 p 101-104 (SEE N88-11609 02-92)

Physics

2

Magnetic Flux, Solar Activity, Solar Magnetic Field, Stellar Interiors, Taylor Instability, Convective Flow, Solar Atmosphere, Solar Cycles, Solar Interior

Scientific paper

In order that magnetic flux be confined within the solar interior for times comparable to the solar cycle period it has been suggested that the bulk of the solar toroidal field is stored in the convectively stable overshoot region situated beneath the convection zone proper. Such a magnetic field, though, is still buoyant and is therefore subject to Rayleigh-Taylor type instabilities. The model problem of an isolated region of magnetic field embedded in a convectively stable atmosphere is considered. The fully nonlinear evolution of the two dimensional interchange of modes is studied, thereby shedding some light on one of the processes responsible for the escape of flux from the solar interior.

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