Neutron Stars—Cooling and Transport

Potekhin, A. Y.; Pons, José A.; Page, Dany

doi:10.1007/978-1-4939-3550-5_8

Cited by 15 publications

(40 citation statements)

References 193 publications

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“…exploited in most works devoted to the NS cooling (for a review, see [11]), where as the most efficient neutrino processes in the NS core are considered the MU processes calculated within the FOPE model [37] and the neutron 3P 2 PBF process calculated following Ref. [102].…”

Section: Resultsmentioning

confidence: 99%

“…Therefore, it is not easy to appropriately explain the essentially different surface temperatures of various objects in the hadronic scenario within the so called "minimal cooling paradigm", cf. [5,8,10,11], where the only relevant rapid process is the so called pair-breakingformation (PBF) process on neutrons paired in the 3P 2 channel. The solution of the puzzle might be associated with a strong medium dependence of cooling inputs, as provided by the densitydependent (and thus neutron star (NS) mass dependent) medium modifications of the N N interaction.…”

Section: Introductionmentioning

confidence: 99%

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Influence of the stiffness of the equation of state and in-medium effects on the cooling of compact stars

2016

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Abstract. Measurements of the low masses for the pulsar PSR J0737-3039B, for the companion of PSR J1756-2251 and for the companion of PSR J0453+1559 on the one hand and of the high masses for the pulsars PSR J1614-2230 and PSR J0348-0432 on the other demonstrate the existence of compact stars with masses in a broad range from 1.2 to 2 M . The most massive of these objects might be hybrid stars. To fulfill the constraint Mmax > 2 M with a reserve we exploit the stiff DD2 hadronic equation of state (EoS) without and with excluded volume (DD2vex) correction, which produce maximum neutron star masses of Mmax = 2.43 M and 2.70 M , respectively. We show that the stiffness of the EoS does not preclude an explanation of the whole set of cooling data within "nuclear medium cooling" scenario for compact stars by a variation of the star masses. We select appropriate proton gap profiles from those exploited in the literature and allow for a variation of the effective pion gap controlling the efficiency of the medium modified Urca process. However, we suppress the possibility of pion condensation. In general, the stiffer the EoS the steeper a decrease with density of the effective pion gap is required. Results are compared with previously obtained ones for the HDD EoS for which Mmax = 2.06 M . The cooling of the compact star in the supernova remnant Cassiopeia A (Cas A) is explained mainly by an efficient medium modified Urca process. To explain a > ∼ 2.5% decline of the cooling curve for Cas A, as motivated by an analysis of the ACIS-S instrument data, together with other cooling data exploiting the DD2 EoS a large proton gap at densities n < ∼ 2n0 is required vanishing for n > ∼ 2.5 n0, where n0 is the saturation nuclear density. A smaller decline, as it follows from an analysis of the HRC-S instrument data, is explained with many choices of parameters. With the DD2vex EoS and using an effective pion gap steeper decreasing with the density and/or a proton gap shifted to smaller densities we are also able to reproduce both a strong decline compatible with ACIS-S data and HRC-S instrument data. The mass of Cas A is estimated as 1.6 − 1.9 M , above the value 1.5 M , which we have evaluated with the softer HDD equation of state. Different mass choices for the hottest object XMMU J173203.3-344518 are discussed. We make general remarks also on hybrid star cooling and on its dependence on the stiffness of the hadronic EoS.PACS. 97.60.Jd Neutron stars -95.30.Cq Elementary particle processes -26.60-c Nuclear matter aspects of neutron stars

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Influence of the stiffness of the equation of state and in-medium effects on the cooling of compact stars

2016

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“…We will use the cooling theory of NSs with nucleon cores and not too strong magnetic fields (to avoid dramatic effects of the B-fields on the NS structure and evolution, such as considered in [10][11][12]). Figure 1 shows some theoretical cooling curves (T ∞ s versus age t) compared with the observations of such (not highly magnetized) NSs.…”

Section: Introductionmentioning

confidence: 99%

Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar

Ofengeim¹,

Zyuzin²

2018

Particles

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Abstract:We reanalyse the X-ray spectrum of the PSR B0833-45 (the Vela pulsar) using the data of the Chandra space observatory. In contrast to previous works, we consider a wide range of possible masses and radii of the pulsar. The derived surface temperature of the star T ∞ s = 0.66−0.01 MK (1σ level over the entire mass and radius range of our study) is consistent with earlier results. However, the preferable values of Vela's mass and radius given by the spectral analysis are different from those used previously; they are consistent with modern equation of state models of neutron star matter. In addition, we evaluate the Vela's surface temperature as a function of assumed values of its mass and radius. This allows us to analyse the neutrino cooling rates consistent with the evaluated surface temperatures and explore the additional restrictions that could be set on the Vela's mass and radius using different versions of the neutron star cooling theory.

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“…In particular, model of neutron star core, consisting of strange quark matter, is discuss and develop at present time [2]. Neutrino cooling of neutron star core is very important, because of such a cooling is responsible for determination and calculation theoretically of neutron star cooling curve [3].…”

Section: Introductionmentioning

confidence: 99%

Direct URCA-processes in neutron star quark core with strong magnetic field.

Belyaev

Gvozdev

2017

EPJ Web Conf.

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Abstract. Neutrino emissivity in direct URCA processes in superdense strongly magnetized quark medium is calculated. In calculations, we use the covariant method of density matrixes for charge fermions in uniform constant magnetic field. One-gluon exchanges between quarks are also take into account. In evaluations, the strength of magnetic field corresponds to the case, where the quarks of medium occupy a lot of Landau levels, while the electrons are in ground Landau level. The analytical dependence of neutrino emissivity on chemical potentials of quarks and electrons, temperature and magnetic field strength is obtained and briefly discussed. The result could be important in application to a massive strongly magnetized neutron star with quark core.

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Neutron Stars—Cooling and Transport

Cited by 15 publications

References 193 publications

Influence of the stiffness of the equation of state and in-medium effects on the cooling of compact stars

Influence of the stiffness of the equation of state and in-medium effects on the cooling of compact stars

Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar

Direct URCA-processes in neutron star quark core with strong magnetic field.

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