Other
Scientific paper
Feb 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...253..290d&link_type=abstract
Astrophysical Journal, Part 1, vol. 253, Feb. 1, 1982, p. 290-297.
Other
91
Dynamo Theory, Late Stars, Magnetohydrodynamics, Stellar Magnetic Fields, Stellar Spectra, Field Strength, Stellar Atmospheres, Stellar Flares, Stellar Rotation
Scientific paper
The principal objective of the present investigation is related to a prediction of the variation of magnetic fields with stellar type and the role of pertinent variables (such as rotation and differential rotation) with respect to the field properties. This is accomplished by estimating a typical amplification time for the magnetic field, and a typical 'time of rise' for the magnetic field due to magnetic buoyancy. It is assumed that the magnetic field is generated principally in the lower part of the stellar convection zone. Local (in latitude) dynamo equations are considered. The selected approach consists basically in an estimate of the typical magnitude of the magnetic field as predicted by the local dynamo equations. The employed approach constitutes only a first step towards the evaluation of magnetic fields in stars other than the sun.
Durney Bernard R.
Robinson Richard D.
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