On the generation of the solar magnetic field in a region of weak buoyancy

Details On the generation of the solar magnetic field in a region of weak buoyancy On the generation of the solar magnetic field in a region of weak buoyancy

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...362..709d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 362, Oct. 20, 1990, p. 709-721.

Astronomy and Astrophysics

Astrophysics

19

Magnetic Flux, Plasma Turbulence, Solar Interior, Solar Magnetic Field, Buoyancy, Temporal Distribution, Turbulence Effects

Scientific paper

The possibility that the cyclic magnetic field of the sun can be generated in a layer of weak buoyancy at the lower boundary of the solar convection zone (SCZ) is addressed using an eddy-damped quasi-normal Markovian closure model of the turbulent MHD equations. It is concluded that only models with kinetic energy of turbulent motion larger than roughly 10 to the 6th g/cm/s are viable. The action of differential rotation on this poloidal field generates a toroidal field exceeding the equipartition value which is sufficiently strong to interfere with the transport of heat and is amplified further in the SCZ.

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