Statistics – Computation
Scientific paper
Sep 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.210..489m&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 210, Sept. 15, 1984, p. 489-495.
Statistics
Computation
4
Magnetic Stars, Molecular Weight, Peculiar Stars, Stellar Evolution, Stellar Magnetic Fields, Stellar Structure, Computational Astrophysics, Magnetic Field Configurations, Main Sequence Stars, Meridional Flow, Stellar Composition, Stellar Models, Stellar Rotation
Scientific paper
Time-dependent magnetic star models are used to examine the effects produced in the magnetic field structure by meridional circulations forced by molecular weight gradients. The star is assumed to have 2.5 solar masses, a 1.6 solar radius, and a brightness of 120 solar luminosities, i.e., a middle main sequence star. Meridional gradients are calculated in the core and at the surface and attention is given to the possibility that a creeping paralysis may occur in the circulation. The paralysis is projected to require longer timescales than the life of a main sequence star. The slow growth rate inhibits significant impacts on the magnetic field structure or its angle relative to the rotation axis.
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