The cooling neutron star in 3C 58

@article{Yakovlev2002TheCN,
  title={The cooling neutron star in 3C 58},
  author={Dmitry Yakovlev and Alexander D. Kaminker and Paweł Haensel and Oleg Y. Gnedin},
  journal={Astronomy and Astrophysics},
  year={2002},
  volume={389}
}
The upper limit on the effective surface temperature of the neutron star (NS) PSR J0205+6449 in the supernova remnant 3C 58 obtained recently by Slane et al. (2002) is analyzed using a modern theory of NS cooling (Kaminker et al. 2002). The observations can be explained by cooling of a superfluid NS with the core composed of neutrons, protons, and electrons, where direct Urca process is forbidden. However, combined with the data on the surface temperatures of other isolated NSs, it gives… 

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References

SHOWING 1-10 OF 23 REFERENCES

Nucleon superfluidity vs. observations of cooling neutron stars

Cooling simulations of neutron stars (NSs) are performed assuming that stellar cores consist of neutrons, protons and electrons and using realistic density proles of superfluid critical temperatures

Three types of cooling superfluid neutron stars: Theory and observations

Cooling of neutron stars (NSs) with the cores composed of neutrons, protons, and electrons is simulated assuming 1 S 0 pairing of neutrons in the NS crust, and also 1 S 0 pairing of protons and weak

Superfluidity in Neutron Star Matter

The research on the superfluidity of neutron matter can be traced back to Migdal’s observation that neutron stars are good candidates for being macroscopic superfluid systems [1]. And, in fact,

Neutrino pair emission from finite-temperature neutron superfluid and the cooling of young neutron stars

The neutrons inside neutron stars are almost certainly superfluid below a critical temperature T/subc/approx.10/sup 10/ K. Below T/subc/, pairs of excited neutron quasiparticles may recombine,

Direct URCA process in neutron stars.

We show that the direct URCA process can occur in neutron stars if the proton concentration exceeds some critical value in the range 11--15%. The proton concentration, which is determined by the

Neutrino emission from neutron stars

Discovery of X-Ray Pulsations from the Compact Central Source in the Supernova Remnant 3C 58

We report on high time and spatial resolution observations of the supernova remnant (SNR) 3C 58 using the High Resolution Camera (HRC) on the Chandra X-Ray Observatory. These data show a pointlike

Physics of Neutron Star Interiors

Microscopic Theory of the Nuclear Equation of State and Neutron Star Structure.- Superfluidity in Neutron Star Matter.- Relativistic Superfluid Models for Rotating Neutron Stars.- The Tensor Virial

A BROADBAND X-RAY STUDY OF THE GEMINGA PULSAR WITH NuSTAR AND XMM-NEWTON

We report on the first hard X-ray detection of the Geminga pulsar above 10 keV using a 150 ks observation with the Nuclear Spectroscopic Telescope Array (NuSTAR) observatory. The double-peaked pulse

1E 1207.4–5209: The Puzzling Pulsar at the Center of the Supernova Remnant PKS 1209–51/52

A second Chandra observation of 1E 1207.4-5209, the central source of the supernova remnant (SNR) PKS 1209-51/52, allowed us to confirm the previously detected period of 424 ms and, assuming a