Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...198..205p&link_type=abstract
Astrophysical Journal, vol. 198, May 15, 1975, pt. 1, p. 205-209.
Astronomy and Astrophysics
Astrophysics
263
Atmospheric Stratification, Dynamo Theory, Magnetic Field Configurations, Magnetic Stars, Solar Magnetic Field, Stellar Rotation, Azimuth, Buoyancy, Convective Flow, Lines Of Force, Magnetic Flux, Solar Activity, Temperature Gradients
Scientific paper
The magnetic field appearing as bipolar magnetic regions at the surface of the sun represents the lines of force from a general azimuthal field of the order of 100 gauss somewhere beneath the surface. The amplification time, as a consequence of the nonuniform rotation, is of the order of 10 years. But magnetic buoyancy brings the azimuthal field up through much of the convective zone in a time rather less than 10 years, raising the question of where the azimuthal field can be retained long enough to be amplified. We show that magnetic fields can be retained for long periods of time in the stable radiative region beneath the convective zone, but unfortunately the solar dynamo cannot function there because turbulent diffusion is an essential part of its operation. The only possible conclusion appears to be that the dynamo operates principally in the very lowest levels of the convective zone at depths of 150,000 km or more, where the gas density is 0.1 g/cu cm, and the fields are limited to 50 gauss.
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