Other
Scientific paper
Sep 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997magn...33..265b&link_type=abstract
Magnetohydrodynamics, Vol. 33, No. 3, p. 265 - 298
Other
Polytropes: Stellar Models, Solar Rotation: Models
Scientific paper
The steady-state (quasi-stationary) solutions for an electromagnetic star in the approximation of an ideally conducting perfect polytropic gas are divided into 4 types. The types 3 and 4 are studied in detail, where the φ-components of the magnetic field strength are of the same order of magnitude as its poloidal components. In the case of the low-frequency steady state oscillations the processes within the internal star layers can be described by means of the quasi-stationary solutions which are nonuniformly applicable along the star radius; the nonuniformity region (low-frequency boundary layer) is localized in the proximity of the star surface. A more general problem of the low-frequency boundary layer is posed, as well as some solutions of the problem are devised, where the angular rotation velocity is of the same order of magnitude as the frequency of the oscillations. Cases are considered, where the angular velocity is much higher than the frequency of the oscillations. Two principles are proposed in order to solve the nonuniqueness problem: the principle of a surface electromagnetic energy minimum over the period of oscillations and the principle of a minimum of the volumetric kinetic energy. The influences of the differential rotation characteristics, as well as of other quantities upon the parameters of the problem are established. Temporal and spatial symmetries of the solution properties are observed which exhibit general differences within the internal regions, as well as at the star surface. The accuracy of the symmetry of solutions is determined as a function of a small parameter. It is noted that the frequency of oscillations on the non-electromagnetic quantities exceeds that of the electromagnetic quantities by a factor of 2.
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