User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse




Journal Article

Gravitational Radiation limit on the Spin of Young Neutron Stars


Schutz,  Bernard F.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Ressource
No external resources are shared
Fulltext (public)

(Any fulltext), 124KB

Supplementary Material (public)
There is no public supplementary material available

Andersson, N., Kokkotas, K. D., & Schutz, B. F. (1999). Gravitational Radiation limit on the Spin of Young Neutron Stars. The Astrophysical Journal, 510, 846-853. doi:10.1086/306625.

Cite as: http://hdl.handle.net/11858/00-001M-0000-0013-7437-1
A newly discovered instability in rotating neutron stars, driven by gravitational radiation reaction acting on the starsœ 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 : in hot neutron stars (T [109 K), the lowest-order r-modes are unstable, while in colder stars they are damped by viscosity. 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 10 and 20 ms. Second, as an initially rapidly rotating star spins down, an energy equivalent to roughly 1% 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 10 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 de–ne the limiting spin period more reliably, and we discuss the importance of the major uncertainties in the stellar models, in the initial conditions after collapse, and in the physics of cooling, super—uidity, and the equation of state.