Statistics – Computation
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.213..575m&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 213, April 1, 1985, p. 575-589.
Statistics
Computation
11
Magnetic Dipoles, Magnetic Stars, Stellar Models, Stellar Rotation, Computational Astrophysics, Dynamo Theory, Magnetic Field Configurations, Stellar Interiors, Time Dependence
Scientific paper
Earlier studies of time-dependent models of rotating magnetic stars are extended to the case where the field is no longer strictly antisymmetric with respect to an equatorial plane, thus modelling the 'displaced dipole' configuration. Results are presented for models which are rotationally dominated, with the meridional flow approximately given by the Eddington-Sweet circulation through most of the radiative region. The angle chi between the rotation and magnetic axes is taken as either 0 or pi/2. When chi = 0 there is critical value of the rotational parameter, lambda(omega), below which an initial field with low concentration to the stellar interior does not change significantly over a main-sequence lifetime. Larger values of lambda(omega) result in a reduction of the surface field with time. When chi = pi/2 the surface field is never buried, but for larger values of lambda(omega) it becomes concentrated towards the magnetic poles.
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