Core-Crust Interaction of Toroidal Modes of Magnetized Neutron Stars

Details Core-Crust Interaction of Toroidal Modes of Magnetized Neutron Stars Core-Crust Interaction of Toroidal Modes of Magnetized Neutron Stars

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..948..263l&link_type=abstract

UNSOLVED PROBLEMS IN STELLAR PHYSICS: A Conference in Honor of Douglas Gough. AIP Conference Proceedings, Volume 948, pp. 263-2

Physics

1

Neutron Stars, Solar Interior, Interplanetary Magnetic Fields, Pulsations, Oscillations, And Stellar Seismology

Scientific paper

We calculate axisymmetric toroidal modes of magnetized neutron stars with a solid crust. We assume the interior of the star is threaded by a poloidal magnetic field that is continuous at the surface with the outside dipole field whose strength Bp at the magnetic pole is Bp~1016 G. Since separation of variables is not possible for oscillations of magnetized stars, to represent the angular dependence of the oscillation modes we employ finite series expansions in terms of spherical harmonic functions. For Bp~1016 G, we find isolated sequences of low radial order toroidal modes, whose oscillation frequency slowly increases as the number of radial nodes of the eigenfunction increases. The frequency spectrum of toroidal modes fox Bp~1016 G is largely different from that of crustal toroidal modes of the non-magnetized model.

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