Thermal conductivity of neutrons in neutron star cores

Baiko, D. A.; Haensel, P.; Yakovlev, D. G.

doi:10.1051/0004-6361:20010621

Cited by 111 publications

(163 citation statements)

References 30 publications

(86 reference statements)

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“…For quark matter κ is the sum of the partial conductivities of the electron, quark and gluon components (Haensel & Jerzak 1989;Baiko & Haensel 1999) …”

Section: Heat Conductivitymentioning

confidence: 99%

Cooling of hybrid neutron stars and hypothetical self-bound objects with superconducting quark cores

Blaschke

Grigorian

Voskresensky³

2001

A&A

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Abstract. We study the consequences of superconducting quark cores (with color-flavor-locked phase as representative example) for the evolution of temperature profiles and cooling curves in quark-hadron hybrid stars and in hypothetical self-bound objects having no hadron shell (quark core neutron stars). The quark gaps are varied from 0 to ∆q = 50 MeV. For hybrid stars we find time scales of 1 ÷ 5, 5 ÷ 10 and 50 ÷ 100 years for the formation of a quasistationary temperature distribution in the cases ∆q = 0, 0.1 MeV and > ∼ 1 MeV, respectively. These time scales are governed by the heat transport within quark cores for large diquark gaps (∆ > ∼ 1 MeV) and within the hadron shell for small diquark gaps (∆ < ∼ 0.1 MeV). For quark core neutron stars we find a time scale 300 years for the formation of a quasistationary temperature distribution in the case ∆ > ∼ 10 MeV and a very short one for ∆ < ∼ 1 MeV. If hot young compact objects will be observed they can be interpreted as manifestation of large gap color superconductivity. Depending on the size of the pairing gaps, the compact star takes different paths in the log(Ts) vs. log(t) diagram where Ts is the surface temperature. Compared to the corresponding hadronic model which well fits existing data the model for the hybrid neutron star (with a large diquark gap) shows too fast cooling. The same conclusion can be drawn for the corresponding self-bound objects.

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“…For quark matter κ is the sum of the partial conductivities of the electron, quark and gluon components (Haensel & Jerzak 1989;Baiko & Haensel 1999) …”

Section: Heat Conductivitymentioning

confidence: 99%

Cooling of hybrid neutron stars and hypothetical self-bound objects with superconducting quark cores

Blaschke

Grigorian

Voskresensky³

2001

A&A

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“…Their mean densityρ ≃ 3M/(4πR 3 ) ≃ 7 × 10 14 g cm −3 is several times the standard nuclear density, ρ 0 = 2.8 × 10 14 g cm −3 . The central density is larger, reaching up to (10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20) ρ 0 . Thus, the cores of neutron stars are composed of a strongly compressed nuclear matter.…”

Section: Introductionmentioning

confidence: 99%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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“…It is higher than the theoretically predicted limit (2). In this case, any cooling neutron star (hidden or unhidden by the SN shell) is so far unobservable.…”

Section: Other Scenariosmentioning

confidence: 64%

“…2, κ is plotted against density in the inner crust and core of a neutron star for two temperatures of matter, T = 10 8 and 10 9 K. The thermal conductivity κ n was calculated using results from Baiko et al (2001). The solid and dashed lines indicate the thermal conductivity in a nonsuperfluid core and in the presence of proton superfluidity, respectively.…”

Section: Cooling Models For Young Neutron Starsmentioning

confidence: 99%

A young cooling neutron star in the remnant of Supernova 1987A

Shternin

Yakovlev

2008

Astron. Lett.

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Abstract-We describe the cooling theory for isolated neutron stars that are several tens of years old. Their cooling differs greatly from the cooling of older stars that has been well studied in the literature. It is sensitive to the physics of the inner stellar crust and even to the thermal conductivity of the stellar core, which is never important at later cooling stages. The absence of observational evidence for the formation of a neutron star during the explosion of Supernova 1987A is consistent with the fact that the star was actually born there. It may still be hidden in the dense center of the supernova remnant. If, however, the star is not hidden, then it should have a low thermal luminosity (below ∼10 34 erg s −1 ) and a short internal thermal relaxation time (shorter than 13 yr). This requires that the star undergo intense neutrino cooling (e.g., via the direct Urca process) and have a thin crust with strong superfluidity of free neutrons and/or an anomalously high thermal conductivity.PACS numbers : 97.58.Mj; 97.60.Jd

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Thermal conductivity of neutrons in neutron star cores

Cited by 111 publications

References 30 publications

Cooling of hybrid neutron stars and hypothetical self-bound objects with superconducting quark cores

Cooling of hybrid neutron stars and hypothetical self-bound objects with superconducting quark cores

Neutrino emission from neutron stars

A young cooling neutron star in the remnant of Supernova 1987A

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