Statistics – Computation
Scientific paper
Jun 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...217..127n&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 217, no. 1-2, June 1989, p. 127-136.
Statistics
Computation
6
Computational Astrophysics, Magnetic Stars, Stellar Magnetic Fields, Stellar Oscillations, Eigenvalues, Equations Of Motion, Force-Free Magnetic Fields, Rayleigh-Ritz Method, Stellar Structure
Scientific paper
The normal modes of oscillation of a perfectly conducting and self-gravitating fluid, pervaded by a force-free magnetic field are studied. A polytropic structure is assumed for the fluid. A gauged version of the Helmholtz theorem is used to decompose the Lagrangian displacements into an irrotational and a weighted solenoidal component. The solenoidal part is further split into poloidal and toroidal components. These components are identified with p, g, and t modes, respectively. The normal modes of the fluid are determined using a Rayleigh-Ritz variational technique. A direct consequence of the presence of the magnetic field is the appearance of t oscillations with periods of the order of Alfven crossing times; these are principally hydromagnetic oscillations. The eigenfrequencies of the ever-present p and g modes are slightly modified. More importantly, however, the later modes acquire a toroidal component, absent in nonmagnetized fluids. The p, g, and t eigenvalues and eigenvectors are computed for different polytropes.
Nasiri Sadolah
Sobouti Yousef
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