Fast rotation of neutron stars and equation of state of dense matter
arXiv:0805.1820 · doi:10.1016/j.newar.2008.03.007
Abstract
Fast rotation of compact stars (at submillisecond period) and, in particular, their stability, are sensitive to the equation of state (EOS) of dense matter. Recent observations of XTE J1739-285 suggest that it contains a neutron star rotating at 1122 Hz (Kaaret et al. 2007). At such rotational frequency the effects of rotation on star's structure are significant. We study the interplay of fast rotation, EOS and gravitational mass of a submillisecond pulsar. We discuss the EOS dependence of spin-up to a submillisecond period, via mass accretion from a disk in a low-mass X-ray binary.
arXiv comment7 pages, 7 figures, proceedings of the "Jean-Pierre Lasota, X-ray binaries, accretion disks and compact stars" conference, edited by M. Abramowicz and O. Straub, New Astronomy Reviews (Elsevier 2008), in press
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Cited by in corpus (9)
- GW190814's secondary component with mass M as a super-fast pulsar
- The High Time Resolution Universe Pulsar Survey VIII: The Galactic millisecond pulsar population
- Effects of the equation of state on the bulk properties of maximally-rotating neutron stars
- Continued Neutron Star Crust Cooling of the 11 Hz X-Ray Pulsar in Terzan 5: A Challenge to Heating and Cooling Models?
- Formation of Sub-millisecond Pulsars and Possibility of Detection
- Stable configurations of hybrid stars with colour-flavour-locked core
- Approximate analytic expressions for circular orbits around rapidly rotating compact stars
- Rotational parameters of strange stars in comparison with neutron stars
- The kHz QPOs of Neutron Stars and Millisecond Pulsars and Implications