Physics
Scientific paper
Jan 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977ap%26ss..46...41d&link_type=abstract
Astrophysics and Space Science, vol. 46, Jan. 1977, p. 41-49.
Physics
17
Convective Flow, Dynamo Theory, Heat Transfer, Solar Atmosphere, Solar Granulation, Solar Magnetic Field, Coriolis Effect, Magnetohydrodynamic Flow, Self Excitation, Solar Physics, Turbulent Diffusion, Turbulent Flow
Scientific paper
A comparison of the equations for magnetic-field and heat transfer by two-dimensional turbulent convection in a conducting compressible medium shows the magnetic field to be transported as a scalar admixture provided it is parallel to the convection cells. At high magnetic Reynolds numbers the field strength in a convection zone varies in proportion to the density of the medium. A study of the distribution and amplification of the poloidal field in the two-dimensional convection zone of the sun and the processes of field pumping and amplification in other zones reveals the importance of considering generation mechanisms of the semidynamo type, where the amplifying field is excited independently by weak emfs of nonelectric origin with no feedback that would otherwise produce MHD self-excitation of the field. A calculation of the solar poloidal field maintained by a weak Coriolis emf acting in a thin external layer of the convective envelope yields for the general near-polar field a value of the order of 0.1 G if allowance is made for field pumping by three-dimensional supergranulation, field transfer and amplification by two-dimensional convection, and ohmic diffusion of the field into a stable core.
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