Properties of high-density matter in neutron stars

Weber, Fridolin; Contrera, Gustavo A.; Orsaria, M.; Spinella, William M.; Zubairi, Omair

doi:10.1142/s0217732314300225

Cited by 33 publications

(34 citation statements)

References 55 publications

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“…In the near future a number of new astrophysical instruments will provide various information on neutron stars (see the recent review [62]). In particular, the Neutron Star Interior Composition Explorer (NICER) [63] to be launched in 2016 is expected to discover tens of thousands of neutron stars and help understanding their core phenomena and to unravel footprints of parity breaking due to pseudoscalar condensation.…”

Section: Discussionmentioning

confidence: 99%

Stellar matter with pseudoscalar condensates

Andrianov¹,

Andrianov²,

Espriu³

et al. 2016

Eur. Phys. J. C

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In this work we consider how the appearance of gradients of pseudoscalar condensates in dense systems may possibly influence the transport properties of photons in such a medium as well as other thermodynamic characteristics. We adopt the hypothesis that in regions where the pseudoscalar density gradient is large the properties of photons and fermions are governed by the usual lagrangian extended with a Chern-Simons interaction for photons and a constant axial field for fermions. We find that these new pieces in the lagrangian produce non-trivial reflection coefficients both for photons and fermions when entering or leaving a region where the pseudoscalar has a non-zero gradient. A varying pseudoscalar density may also lead to instability of some fermion and boson modes and modify some properties of the Fermi sea. We speculate that some of these modifications could influence the cooling rate of stellar matter (for instance in compact stars) and have other observable consequences. While quantitative results may depend on the precise astrophysical details most of the consequences are quite universal and consideration should be given to this possibility.

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Section: Discussionmentioning

confidence: 99%

Stellar matter with pseudoscalar condensates

Andrianov¹,

Andrianov²,

Espriu³

et al. 2016

Eur. Phys. J. C

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“…Here 2 is the neutrino transverse momenta squared and integrals I n,m i are determined, as follows: From this point we use various approximations. First, we assume, that the parameter v 2 = k 2 ⊥ /eB is small (v 1).…”

Section: Integrals On Transversal To Magnetic Field Strength Componenmentioning

confidence: 99%

“…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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“…The question of whether or not quark matter exists in neutron stars has received renewed interest (see Refs., [1][2][3] and references therein) by the discovery of the two massive neutron stars (NS) J1614-2230 (1.97±0.04M (see Ref. 4 ), recently updated to 1.928 ± 0.017M (see Ref.…”

Section: Introductionmentioning

confidence: 99%

Hybrid Stars in the Framework of NJL Models

Contrera

Orsaria

Ranea‐Sandoval

et al. 2017

Int. J. Mod. Phys. Conf. Ser.

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This is an Open Access article published by World Scientific Publishing Company. It is distributed under the terms of the Creative Commons Attribution 4.0 (CC-BY) License. Further distribution of this work is permitted, provided the original work is properly cited. G. A. Contrera et al.We compute models for the equation of state (EoS) of the matter in the cores of hybrid stars. Hadronic matter is treated in the non-linear relativistic mean-field approximation, and quark matter is modeled by three-flavor local and non-local Nambu−Jona-Lasinio (NJL) models with repulsive vector interactions. The transition from hadronic to quark matter is constructed by considering either a soft phase transition (Gibbs construction) or a sharp phase transition (Maxwell construction). We find that high-mass neutron stars with masses up to 2.1 − 2.4M may contain a mixed phase with hadrons and quarks in their cores, if global charge conservation is imposed via the Gibbs conditions. However, if the Maxwell conditions is considered, the appearance of a pure quark matter core either destabilizes the star immediately (commonly for non-local NJL models) or leads to a very short hybrid star branch in the mass-radius relation (generally for local NJL models).

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Properties of high-density matter in neutron stars

Cited by 33 publications

References 55 publications

Stellar matter with pseudoscalar condensates

Stellar matter with pseudoscalar condensates

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

Hybrid Stars in the Framework of NJL Models

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