Description
This talk investigates the spin-up evolution of accreting neutron stars into millisecond pulsars. Relativistic stellar models are generated by a numerical implementation of Hartle's perturbative axisymmetric solutions to Einstein's field equations for various equations of state. With a hydrodynamic model of asymptotic magnetic field decay, the bulk properties of evolution over time are investigated by means of an evolution equation derived from a classical accretion model developed by Ghosh and Lamb et. al. A computational study of the overall spin-up behavior shows a necessity for general relativistic stellar models that account for changing moments of inertia with gravitational mass in simulations over long durations. Moreover, a rapid spin-up followed by a gradual spin-down with heavy mass loading with increasing central density are demonstrated for high accretion rates
