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The evolution of the r-mode instability is likely to be accompanied bysecular kinematic effects which will produce differential rotation with largescale drifts of fluid elements, mostly in the azimuthal direction. As firstdiscussed by Rezzolla, Lamb and Shapiro 2000, the interaction of these secularvelocity fields with a pre-existing neutron star magnetic field could result inthe generation of intense and large scale toroidal fields. Following theirderivation in the companion paper, we here discuss the numerical solution ofthe evolution equations for the magnetic field. The values of the magneticfields obtained in this way are used to estimate the conditions under which ther-mode instability might be prevented or suppressed. We also assess the impactof the generation of large magnetic fields on the gravitational wavedetectability of r-mode unstable neutron stars. Our results indicate that thesignal to noise ratio in the detection of gravitational waves from the r-modeinstability might be considerably decreased if the latter develops in neutronstars with initial magnetic fields larger than 10^10 G.Comment: 16 pages, 12 figures. To appear in Phys. Rev.

physical review. d. particles, fields, gravitation, and cosmology/physical review. d. particles and fields

Properties of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>r</mml:mi></mml:math>modes in rotating magnetic neutron stars. II. Evolution of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>r</mml:mi></mml:math>modes and stellar magnetic field

Properties ofrmodes in rotating magnetic neutron stars. II. Evolution of thermodes and stellar magnetic field