The large-scale internal solar magnetic field

Details The large-scale internal solar magnetic field The large-scale internal solar magnetic field

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989azh....66..809d&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 66, July-Aug. 1989, p. 809-821. In Russian.

Astronomy and Astrophysics

Astronomy

8

Dynamo Theory, Magnetohydrodynamics, Solar Interior, Solar Magnetic Field, Solar Radiation, Convection, Rotating Matter, Star Formation, Stellar Evolution

Scientific paper

It is hypothesized that, during the collapse of the protosolar cloud, the magnetic field intensified. In the center of the just-formed, nonturbulent sun, the intensity of the magnetic field was 10,000 to 1 million G. If the sun passed through a stage of turbulent convection, only the field generated by dynamo action would remain. The poloidal magnetic field at this stage could reach 1000-1,000,000 G, but the intensity would decrease to 10-1 G during the decay of turbulent convection. The toroidal magnetic field would remain at 1000-1,000,000 G. It is possible that nonuniform rotation of the radiative region is related to distortions in the angular velocity in the internal convective zone due to magnetic tension.

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