Neutron star news and puzzles

@article{Prakash2014NeutronSN,
  title={Neutron star news and puzzles},
  author={Madappa Prakash},
  journal={Nuclear Physics},
  year={2014},
  volume={928},
  pages={260-275}
}
  • M. Prakash
  • Published 7 April 2014
  • Physics
  • Nuclear Physics
1 Citations

R-mode constraints from neutron star equation of state

The gravitational radiation has been proposed a long time before, as an explanation for the observed relatively low spin frequencies of young neutron stars and of accreting neutron stars in low-mass

References

SHOWING 1-10 OF 90 REFERENCES

RX J1856: astrophysical evidence for quark stars

On 10 April 2002 NASA announced that Chandra observations of the compact object RX J185635-3754 implied that it was smaller than allowed by models of neutron stars, and that this was evidence for the

A two-solar-mass neutron star measured using Shapiro delay

Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state.

Cooling neutron star in the Cassiopeia A supernova remnant: evidence for superfluidity in the core

According to recent results of Ho & Heinke, the Cassiopeia A supernova remnant contains a young (?330-yr-old) neutron star (NS) which has carbon atmosphere and shows notable decline of the effective

The Physics of Neutron Stars

Observations that include studies of pulsars in binary systems, thermal emission from isolated neutron stars, glitches from pulsars, and quasi-periodic oscillations from accreting neutron stars provide information about neutron star masses, radii, temperatures, ages, and internal compositions.

Constraints on neutron star radii based on chiral effective field theory interactions.

We show that microscopic calculations based on chiral effective field theory interactions constrain the properties of neutron-rich matter below nuclear densities to a much higher degree than is

Stellar Superfluids

Neutron stars provide a fertile environment for exploring superfluidity under extreme conditions. It is not surprising that Cooper pairing occurs in dense matter since nucleon pairing is observed in

Cooling of the neutron star in Cassiopeia A

We demonstrate that the high-quality cooling data observed for the young neutron star in the supernova remnant Cassiopeia A over the past 10 years---as well as all other reliably known temperature

Forecasting neutron star temperatures: predictability and variability.

It is now possible to model thermal relaxation of neutron stars after bouts of accretion during which the star is heated out of equilibrium by nuclear reactions in its crust, and observations of thermal relaxation constrain these parameters and allow us to predict longer term variability in terms of the neutron star core temperature.

CONTINUED COOLING OF THE CRUST IN THE NEUTRON STAR LOW-MASS X-RAY BINARY KS 1731−260

A new Chandra observation of KS 1731-260 finds that the source has continued to cool, with the cooling curve displaying a simple power-law decay, suggesting that the crust has not fully thermally relaxed yet and may continue to cool further.

A Massive Pulsar in a Compact Relativistic Binary

Introduction Neutron stars with masses above 1.8 solar masses (M☉), possess extreme gravitational fields, which may give rise to phenomena outside general relativity. These strong-field deviations
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