Rotation at 1122 Hz and the neutron star structure

@article{Bejger2007RotationA1,
  title={Rotation at 1122 Hz and the neutron star structure},
  author={Michał Bejger and Paweł Haensel and Julian Leszek Zdunik},
  journal={Astronomy and Astrophysics},
  year={2007},
  volume={464}
}
Aims. Recent observations of XTE J1739-285 suggest that it contains a neutron star rotating at 1122 Hz. Such rotation imposes bounds on the structure of neutron star in XTE J1739-285. These bounds may be used to constrain poorly known equation of state of dense matter at densities ${\ga} 10^{15}~{\rm g~cm^{-3}}$. Methods. One-parameter families of stationary configurations rotating rigidly at 1122 Hz are constructed, using a precise 2D code solving Einstein equations. Hydrostatic equilibrium… 

Figures and Tables from this paper

Does Submillisecond Pulsar XTE J1739-285 Contain a Weak Magnetic Neutron Star or Quark Star?
The possible detection of the fastest spinning nuclear-powered pulsar XTE J1739–285, of frequency 1122 Hz (0.8913 ms), arouses us to constrain the mass and radius of its central compact object and to
Rotating neutron stars with exotic cores: masses, radii, stability
Abstract.A set of theoretical mass-radius relations for rigidly rotating neutron stars with exotic cores, obtained in various theories of dense matter, is reviewed. Two basic observational
Constraining Properties of Rapidly Rotating Neutron Stars Using Data from Heavy-Ion Collisions
Properties, structure, and thermal evolution of neutron stars are determined by the equation of state of stellar matter. Recent data on isospin diffusion and isoscaling in heavy-ion collisions at
Fundamental physics and the absence of sub-millisecond pulsars
Context. Rapidly rotating neutron stars are an ideal laboratory to test models of matter at high densities. In particular, the maximum rotation frequency of a neutron star depends on the equation of
Nonrotating and rotating neutron stars in the extended field theoretical model
We study the properties of nonrotating and rotating neutron stars for a new set of equations of state (EOSs) with different high-density behavior obtained using the extended field theoretical model.
Keplerian frequency of uniformly rotating neutron stars and strange stars
Aims. We calculate Keplerian (mass shedding) configurations of rigidly rotating neutron stars and strange stars with crusts. We check the validity of the empirical formula for Keplerian frequency, f
Parameters of rotating neutron stars with and without hyperons
The discovery of a 2 Msun neutron star provided a robust constraint for the theory of exotic dense matter, bringing into question the existence of strange baryons in the interiors of neutron stars.
A Compact Star Rotating at 1122 Hz and the r-Mode Instability
We show that r-mode instabilities severely constrain the composition of a compact star rotating with a submillisecond period. In particular, the only viable astrophysical scenario for such an object,
Correlations in the properties of static and rapidly rotating compact stars
Correlations in the properties of the static compact stars (CSs) and the ones rotating with the highest observed frequency of 1122 Hz are studied using a large set of equations of state (EOSs). These
Equation of state at high densities and modern compact star observations
Recently, observations of compact stars have provided new data of high accuracy which put strong constraints on the high-density behaviour of the equation of state of strongly interacting matter
...
...

References

SHOWING 1-10 OF 29 REFERENCES
Rapidly Rotating Neutron Stars in General Relativity: Realistic Equations of State
We construct equilibrium sequences of rotating neutron stars in general relativity. We compare results for fourteen nuclear matter equations of state. We determine a number of important physical
Equation of state of nucleon matter and neutron star structure
Properties of dense nucleon matter and the structure of neutron stars are studied using variational chain summation methods and the new Argonne ${v}_{18}$ two-nucleon interaction, which provides an
Are rotating strange quark stars good sources of gravitational waves
We study the viscosity driven (Jacobi-like) bar mode instability of rapidly rotating strange stars in general relativity. A triaxial, "bar shaped" compact star could be an efficient source of
Implications of the millisecond pulsar for neutron star models
We examine the constraints imposed by the high spin rate of PSR 1937+214 on the masses and radii of nonrotating neutron stars that can be spun up to such a short period. Assuming uniform rotation, we
A unified equation of state of dense matter and neutron star structure
An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated. It is based on the eective nuclear interaction SLy of the Skyrme type,
A Radio Pulsar Spinning at 716 Hz
TLDR
A 716-hertz eclipsing binary radio pulsar in the globular cluster Terzan 5 using the Green Bank Telescope is discovered, it is the fastest spinning neutron star found to date, and constrains models that suggest that gravitational radiation, through an r-mode (Rossby wave) instability, limits the maximum spin frequency of neutron stars.
A 2.1 M☉ Pulsar Measured by Relativistic Orbital Decay
PSR J0751+1807 is a millisecond pulsar in a circular 6 hr binary system with a helium white dwarf secondary. Through high-precision pulse timing measurements with the Arecibo and Effelsberg radio
Construction of highly accurate models of rotating neutron stars: Comparison of three different numerical schemes
TLDR
The codes can be used for theruction of highly accurate initial data congurations for polytropes of index N> 0 :5 (which typically correspond to realistic neutron stars), when the domain of integra- tion includes all space and for realistic equations with no phase transitions.
Superbursts from Strange Stars
Recent models of carbon ignition on accreting neutron stars predict superburst ignition depths that are an order of magnitude larger than those observed. We explore a possible solution to this
A millisecond pulsar
TLDR
The puzzle of the radio properties of 4C21.53 may be resolved by the discovery and related observations of a fast pulsar, 1937+214, with a period of 1.558 ms in the constellation Vulpecula only a few degrees from the direction to the original pulsar.
...
...