GRAVITATIONAL RADIATION LIMIT ON THE SPIN OF YOUNG NEUTRON STARS

摘要

A newly discovered instability in rotating neutron stars, driven by gravitational radiation reaction acting on the stars' r-modes, is shown here to set an upper limit on the spin rate of young neutron stars, We calculate the timescales for the growth of linear perturbations due to gravitational radiation reaction, and for dissipation by shear and bulk viscosity, working to second order in a slow-rotation expansion within a Newtonian polytropic stellar model. The results are very temperature-sensitive f in hot neutron stars (T > l0~9 K), the lowest-order r-modes are unstable, while in colder stars they are damped by vis- cosity. These calculations have a number of interesting astrophysical implications. First, the r-mode instability will spin down a newly born neutron star to a period close to the initial period inferred for the Crab pulsar, probably between l0 and 20 ms. Second, as an initially rapidly rotating star spins down, an energy equiva1ent to roughly l of a solar, mass is radiated as gravitational waves, which makes the process an interesting source for detectable gravitational waves. Third, the r-mode instability rules out the scenario in which millisecond pulsars are formed by accretion-induced collapse of a white dwarf, the new star would be hot enough to spin down to much slower rates. Stars with periods less than perhaps l0 ms must have been formed by spin-up through accretion in binary systems, where they remain colder than the Eddington temperature of about 108 K. More accurate calculations will be required to define the limiting spin period more reliably,