Evolution of a magnetic flux tube in two-dimensional penetrative convection

Details Evolution of a magnetic flux tube in two-dimensional penetrative convection Evolution of a magnetic flux tube in two-dimensional penetrative convection

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.259..465j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 259, no. 3, p. 465-473.

Astronomy and Astrophysics

Astronomy

8

Solar Convection (Astronomy), Solar Interior, Solar Magnetic Field, Solar Rotation, Stellar Models, Sunspots, Traveling Waves

Scientific paper

Highly supercritical compressible convection is simulated in a two-dimensional domain in which the upper half is unstable to convection while the lower half is stably stratified. This configuration is an idealization of the layers near the base of the solar convection zone. Once the turbulent flow is well developed, a toroidal magnetic field Btor is introduced to the stable layer. The field's evolution is governed by an advection-diffusion-type equation, and the Lorentz force does not significantly affect the flow. After many turnover times the field is stratified such that the absolute value of Btor/rho is approximately constant in the convective layer, where rho is density, while in the stable layer this ratio decreases linearly with depth. Consequently most of the magnetic flux is stored in the overshoot layer. The inclusion of rotation leads to travelling waves which transport magnetic flux latitudinally in a manner reminiscent of the migrations seen during the solar cycle.

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