Publication Date:
2019-06-28
Description:
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.
Keywords:
SOLAR PHYSICS
Type:
NASA-Goddard Space Flight Center, Theoretical Problems in High Resolution Solar Physics, 2; p 101-104
Format:
application/pdf
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