The magnetic field transfer in the solar convective zone

Details The magnetic field transfer in the solar convective zone The magnetic field transfer in the solar convective zone

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ap%26ss..57..195r&link_type=abstract

Astrophysics and Space Science, vol. 57, no. 1, Aug. 1978, p. 195-202.

Astronomy and Astrophysics

Astrophysics

5

Convective Flow, Magnetic Field Configurations, Magnetohydrodynamic Turbulence, Plasma Turbulence, Solar Magnetic Field, Buoyancy, Density Distribution, Diamagnetism, Dynamo Theory, Turbulence Effects

Scientific paper

The large-scale azimuthal magnetic field is pumped to the bottom of the solar convection zone due to the diamagnetic action of turbulent conductive fluids. When the field at the bottom is about 1000 G, an equilibrium is established between diamagnetic pumping and buoyancy. If, in addition to the density gradient, an additional anisotropy exists (for instance, due to rotation), another mechanism of magnetic-field transfer operates, the efficiency of which greatly depends on the magnitude of the anisotropy parameter.

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