Properties of r modes in rotating magnetic neutron stars. I. Kinematic secular effects and magnetic evolution equations - art. no. 104013

The instability of r-mode oscillations in rapidly rotating neutron stars ha s attracted attention as a potential mechanism for producing high frequency , almost periodic gravitational waves. The analyses carried so far have sho wn the existence of these modes and have considered damping by shear and bu lk viscosity. However, the magnetohydrodynamic coupling of the modes with a stellar magnetic field and its role in the damping of the instability has not been fully investigated yet. Following our introductory paper [L. Rezzo lla, F. K Lamb, and S. L. Shapiro, Astrophys. J. Lett. 531, L141 (2000)], w e here discuss in more detail the existence of secular higher-order kinemat ical effects which will produce toroidal fluid drifts. We also define the s ets of equations that account for the time evolution of the magnetic fields produced by these secular velocity fields and show that the magnetic field s produced can reach equipartition in less than a year. The full numerical calculations as well as them evaluation of the impact of strong magnetic fi elds on the onset and evolution of the r-mode instability will be presented in a companion paper [L. Rezzolla, F. K. Lamb, D. Markovic, and S. L. Shap iro, following paper, Phys. Rev. D 64, 104014 (2001)].