r-mode runaway and rapidly rotating neutron stars

We present a simple spin-evolution model that predicts that rapidly rotatin g accreting neutron stars will be confined mainly to a narrow range of spin frequencies: P = 1.5-5 ms. This is in agreement with current observations of neutron stars in both the low-mass X-ray binaries and the millisecond ra dio pulsars. The main ingredients in the model are (1) the instability of r -modes above a critical spin rate, (2) the thermal runaway that is due to t he heat released as viscous damping mechanisms counteract the r-mode growth , and (3) a revised estimate of the strength of the dissipation that is due to the presence of a viscous boundary layer at the base of the crust in an old and relatively cold neutron star. We discuss the gravitational waves t hat are radiated during the brief r-mode-driven spin-down phase. We also br iefly touch on how the new estimates affect the predicted initial spin peri ods of hot young neutron stars.