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We study the spindown of isolated neutron stars from initially rapid rotationrates, driven by two factors: (i) gravitational wave emission due to r-modesand (ii) magnetic braking. In the context of isolated neutron stars, we presentthe first study including self-consistently the magnetic damping of r-modes inthe spin evolution. We track the spin evolution employing the RNS code, whichaccounts for the rotating structure of neutron stars for various equations ofstate. We find that, despite the strong damping due to the magnetic field,r-modes alter the braking rate from pure magnetic braking for B<10^{13}G. Forrealistic values of the saturation amplitude, the r-mode can also decrease thetime to reach the threshold central density for quark deconfinement. Within aphenomenological model, we assess the gravitational waveform that would resultfrom r-mode driven spindown of a magnetized neutron star. To contrast with thepersistent signal during the spindown phase, we also present a preliminaryestimate of the transient gravitational wave signal from an explosivequark-hadron phase transition, which can be a signal for the deconfinement ofquarks inside neutron stars.

Spindown of Isolated Neutron Stars: Gravitational Waves or Magnetic Braking?