Self-similarity relations for cooling superfluid neutron stars

Shternin, P. S.; Yakovlev, D. G.

doi:10.1093/mnras/stu2339

Cited by 21 publications

(52 citation statements)

References 21 publications

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“…The neutron contribution (the left panel of Fig. 5) is accurately reproduced by the approximation (21). It is precise enough to distinguish between very close C n − M relations for different EOSs.…”

Section: Calculation Of the Neutrino Luminosity And Heat Capacitymentioning

confidence: 58%

Neutrino luminosities and heat capacities of neutron stars in analytic form

et al. 2017

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We derive analytic approximations for the neutrino luminosities and the heat capacities of neutron stars with isothernal nucleon cores as functions of the mass and radius of stars. The neutrino luminosities are approximated for the three basic neutrino emission mechanisms, and the heat capacities for the five basic combinations of the partial heat capacities. The approximations are valid for for a wide class of equations of state of dense nucleonmatter. The results significantly simplify the theoretical interpretation of observations of cooling neutron stars as well as of quasistationary thermal states of neutron stars in X-ray transients. For illustration, we present an analysis of the neutrino cooling functions of nine isolated neutron stars taking into account the effects of their magnetic fields and of the presence of light elements in their heat blanketing envelopes. These results allow one to investigate the superfluid properties of neutron star cores.

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Section: Calculation Of the Neutrino Luminosity And Heat Capacitymentioning

confidence: 58%

Neutrino luminosities and heat capacities of neutron stars in analytic form

et al. 2017

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“…[29,30,31]. Future work will use the new results to further improve our knowledge of nuclear physics properties (see, e.g., [41,42]).…”

Section: Discussionmentioning

confidence: 99%

Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning

Wijngaarden

Chang

et al. 2019

AIP Conference Proceedings

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The study of how neutron stars cool over time can provide invaluable insights into fundamental physics such as the nuclear equation of state and superconductivity and superfluidity. A critical relation in neutron star cooling is the one between observed surface temperature and interior temperature. This relation is determined by the composition of the neutron star envelope and can be influenced by the process of diffusive nuclear burning (DNB). We calculate models of envelopes that include DNB and find that DNB can lead to a rapidly changing envelope composition which can be relevant for understanding the long-term cooling behavior of neutron stars. We also report on analysis of the latest temperature measurements of the young neutron star in the Cassiopeia A supernova remnant. The 13 Chandra observations over 18 years show that the neutron star's temperature is decreasing at a rate of 2-3% per decade, and this rapid cooling can be explained by the presence of a proton superconductor and neutron superfluid in the core of the star.

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“…(14) can still be used supplied with the superfluid suppression factors [6]. Notice, that in the same region, the situation is further complicated by the appearance of the neutrino emission associated with the Cooper pair formation processes [40,41,42,8]. The detailed treatment of the superfluid case is outside the scope of the present paper and we plan to address the effects of superfluidity in the future work.…”

Section: Discussionmentioning

confidence: 99%

In-medium enhancement of the modified Urca neutrino reaction rates

2018

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We calculate modified Urca neutrino emission rates in the dense nuclear matter in neutron star cores. We find that these rates are strongly enhanced in the beta-stable matter in regions of the core close to the direct Urca process threshold. This enhancement can be tracked to the use of the in-medium nucleon spectrum in the virtual nucleon propagator. We describe the in-medium nucleon scattering in the non-relativistic Bruckner-Hartree-Fock framework taking into account two-body as well as the effective threebody forces, although the proposed enhancement does not rely on a particular way of the nucleon interaction treatment. Finally we suggest a simple approximate expression for the emissivity of the neutron branch of the modified Urca process that can be used in the neutron stars cooling simulations with any nucleon equation of state of dense matter.

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Self-similarity relations for cooling superfluid neutron stars

Cited by 21 publications

References 21 publications

Neutrino luminosities and heat capacities of neutron stars in analytic form

Neutrino luminosities and heat capacities of neutron stars in analytic form

Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning

In-medium enhancement of the modified Urca neutrino reaction rates

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