Implication of existence of hybrid stars and theoretical expectation of submillisecond pulsars

  title={Implication of existence of hybrid stars and theoretical expectation of submillisecond pulsars},
  author={Xiaoping Zheng and Na-na Pan and Shu-Hua Yang and Xuewen Liu and Miao Kang and Jia-rong Li},
  journal={New Astronomy},
Abstract We derive the bulk viscous damping timescale of hybrid stars, neutron stars with quark matter core. The r -mode instability windows of the stars show that the theoretical results are consistent with the rapid rotation pulsar data, which may give an indication for the existence of quark matter in the interior of neutron stars. Hybrid stars instead of neutron or strange stars may lead to submillisecond pulsars. 

Figures and Tables from this paper

Thermal Evolution of Strange Stars
We have investigated the thermal evolution of rotating strange stars with the deconfinement heating due to magnetic braking. We consider stars consisting of either normal quark matter or a
The formation of submillisecond pulsars and the possibility of detection
Pulsars have been recognized to be normal neutron stars, but sometimes have been argued to be quark stars. Submillisecond pulsars, if detected, would play an essential and important role in
Viscous damping of r-mode oscillations in compact stars with quark matter.
We determine characteristic time scales for the viscous damping of r-mode oscillations in rapidly rotating compact stars that contain quark matter. We present results for the color-flavor-locked
1122 Hz rotation of XTE J1739-285 as a probe of quark matter in the interior of the neutron star
The recent discovery of burst oscillation at 1122Hz in the X-ray transient XTE J1739-285 supports the suggestion that it contains a submillisecond pulsar. In our estimations of the enormous


Probing strange stars and color superconductivity by r-mode instabilities in millisecond pulsars
  • Madsen
  • Physics, Medicine
    Physical review letters
  • 2000
r-mode instabilities in rapidly rotating quark matter stars (strange stars) lead to specific signatures in the evolution of pulsars with periods below 2.5 msec, and may explain the apparent lack of
Bulk viscosity of strange quark matter, damping of quark star vibration, and the maximum rotation rate of pulsars.
  • Madsen
  • Physics, Medicine
    Physical review. D, Particles and fields
  • 1992
The bulk viscosity of strange quark matter is calculated in the light of new rate expressions for the reaction u+s ↔ d+u, implying rapid damping of stellar vibrations and suppression of nonaxisymmetric instabilities for rapidly spinning pulsars.
Contrary to young neutron stars, young strange stars are not subject to the r-mode instability which slows rapidly rotating, hot neutron stars to rotation periods near 10 ms via gravitational wave
In this review we summarize the current understanding of the gravitational-wave driven instability associated with the so-called r-modes in rotating neutron stars. We discuss the nature of the
The Critical Rotation of Strange Stars and Rapidly Rotating Pulsars
We utilize the bulk viscosity of interacting strange quark matter to reevaluate the damping timescale. The presence of a medium effect of bulk viscosity leads to a stronger damping of r-modes, which
Effect of hyperon bulk viscosity on neutron-star r-modes
Neutron stars are expected to contain a significant number of hyperons in addition to protons and neutrons in the highest density portions of their cores. Following the work of Jones, we calculate
Runaway Heating by r-Modes of Neutron Stars in Low-Mass X-Ray Binaries
Recently Andersson et al. and Bildsten have independently suggested that an r-mode instability might be responsible for stalling the neutron star spin-up in strongly accreting low-mass X-ray binaries
Axial instability of rotating relativistic stars
Perturbations of rotating relativistic stars can be classified by their behavior under parity. For axial perturbations (r-modes), initial data with negative canonical energy is found with angular
The Oscillations of Rapidly Rotating Newtonian Stellar Models. II. Dissipative Effects
A method is described for determining the dissipative effects of viscosity and gravitational radiation on the modes of rapidly rotating Newtonian stellar models. Integral formulae for the dissipative
Hybrid stars and quark hadron phase transition in chiral colour dielectric model
We investigate the properties of hybrid stars consisting of quark matter in the core and hadron matter in outer region. The hadronic equation of state (EOS) is calculated by using nonlinear Walecka