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R-modes in the ocean of a magnetic neutron star

Vahid Rezania
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Abstract

We study the dynamics of r-modes in the ocean of a magnetic neutron star. We modeled the star's ocean with a spherical rotating thin shell and assumed that the magnetic field symmetry axis is not aligned to the shell's spin axis. In the magnetohydrodynamic approximation, we calculate the frequency of $\ell=m$ r-modes in the shell of an incompressible fluid. Different r-modes with $\ell$ and $\ell\pm2$ are coupled by the {\it inclined} magnetic field. Kinematical secular effects for the motion of a fluid element in the shell undergoing $\ell=m=2$ r-mode are studied. The magnetic corrected drift velocity of a given fluid element undergoing the $\ell=m$ r-mode oscillations is obtained. The magnetic field increases the magnitude of the fluid drift produced by the r-mode drift velocity, the high-$\ell$ modes in the ocean fluid will damp faster than the low-$\ell$ ones.

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Vahid Rezania. 2002-04-09. R-modes in the ocean of a magnetic neutron star. https://doi.org/10.1086/341115

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