TY - JOUR

T1 - Axisymmetric toroidal modes of magnetized neutron stars

AU - Lee, Umin

PY - 2008/4

Y1 - 2008/4

N2 - 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 ∼ 10 16 G. Since separation of variables is not possible for oscillations of magnetized stars, we employ finite series expansions of the perturbations using spherical harmonic functions to represent the angular dependence of the oscillation modes. For Bp ∼ 1016 G, we find discrete normal toroidal modes which form distinct mode sequences, in each of which the oscillation frequency of the toroidal mode slowly increases as the number of radial nodes of the eigenfunction increases. The frequency spectrum of the toroidal modes for Bp ∼ 1016 G is largely different from that of the crustal toroidal modes of the non-magnetized model, although the frequency ranges are overlapped each other. This suggests that an interpretation of the observed quasi-periodic oscillations (QPOs) based on the magnetic toroidal modes may be possible if the field strength of the star is as strong as Bp ∼ 1016 G.

AB - 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 ∼ 10 16 G. Since separation of variables is not possible for oscillations of magnetized stars, we employ finite series expansions of the perturbations using spherical harmonic functions to represent the angular dependence of the oscillation modes. For Bp ∼ 1016 G, we find discrete normal toroidal modes which form distinct mode sequences, in each of which the oscillation frequency of the toroidal mode slowly increases as the number of radial nodes of the eigenfunction increases. The frequency spectrum of the toroidal modes for Bp ∼ 1016 G is largely different from that of the crustal toroidal modes of the non-magnetized model, although the frequency ranges are overlapped each other. This suggests that an interpretation of the observed quasi-periodic oscillations (QPOs) based on the magnetic toroidal modes may be possible if the field strength of the star is as strong as Bp ∼ 1016 G.

KW - Stars: magnetic fields

KW - Stars: neutron

KW - Stars: oscillations

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U2 - 10.1111/j.1365-2966.2008.12965.x

DO - 10.1111/j.1365-2966.2008.12965.x

M3 - Article

AN - SCOPUS:41849149291

VL - 385

SP - 2069

EP - 2079

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -