Quark beta decay in the inhomogeneous chiral phase and cooling of compact stars

Tatsumi, Toshitaka; Muto, Takumi

doi:10.1103/physrevd.89.103005

Cited by 18 publications

(22 citation statements)

References 62 publications

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“…It is therefore highly desirable to work out more sensitive signatures of their formation. A first example in this direction is the neutrino emissivity, discussed in [69], which is related to the cooling properties of the star. A complete calculation of the cooling process of the whole star would however be required before a detailed comparison with astrophysical data could be made.…”

Section: Discussionmentioning

confidence: 99%

“…The authors of ref. [69] therefore conclude that heavier stars may not cool faster than lighter ones.…”

Section: Neutrino Emissivitymentioning

confidence: 99%

“…An exception is the neutrino emissivity, which has been worked out for a CDW in ref. [69]. This will be reviewed in sect.…”

Section: Astrophysical Implications Of Inhomogeneous Chiral Symmetry mentioning

confidence: 99%

“…This scenario has been worked out in detail in [69], where the neutrino emissivity (i.e. the emitted energy per unit volume and time) has been calculated for the case of a CDW modulation (eq.…”

Section: Neutrino Emissivitymentioning

confidence: 99%

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Inhomogeneous chiral symmetry breaking in dense neutron-star matter

Buballa

Carignano

2016

Eur. Phys. J. A

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Abstract. An increasing number of model results suggests that chiral symmetry is broken inhomogeneously in a certain window at intermediate densities in the QCD phase diagram. This could have significant effects on the properties of compact stars, possibly leading to new astrophysical signatures. In this contribution we discuss this idea by reviewing recent results on inhomogeneous chiral symmetry breaking under an astrophysics-oriented perspective. After introducing two commonly studied spatial modulations of the chiral condensate, the chiral density wave and the real kink crystal, we focus on their properties and their effect on the equation of state of quark matter. We also describe how these crystalline phases are affected by different elements which are required for a realistic description of a compact star, such as charge neutrality, the presence of magnetic fields, vector interactions and the interplay with color superconductivity. Finally, we discuss possible signatures of inhomogeneous chiral symmetry breaking in the core of compact stars, considering the cases of mass-radius relations and neutrino emissivity explicitly.PACS. 26.60.-c Nuclear matter aspects of neutron stars

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Section: Discussionmentioning

confidence: 99%

“…The authors of ref. [69] therefore conclude that heavier stars may not cool faster than lighter ones.…”

Section: Neutrino Emissivitymentioning

confidence: 99%

“…An exception is the neutrino emissivity, which has been worked out for a CDW in ref. [69]. This will be reviewed in sect.…”

Section: Astrophysical Implications Of Inhomogeneous Chiral Symmetry mentioning

confidence: 99%

Section: Neutrino Emissivitymentioning

confidence: 99%

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Inhomogeneous chiral symmetry breaking in dense neutron-star matter

Buballa

Carignano

2016

Eur. Phys. J. A

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“…Ref. [7] proposes that the existence of an inhomogeneous chiral phase leads to a novel cooling scenario for neutron stars, finding a neutrino emissivity with efficiency comparable with the usual quark cooling or pion cooling. Consequences of an inhomogeneous chiral phase for the equation of state of matter in neutron stars have been investigated in Refs.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of inhomogeneous chiral condensates

Carlomagno

Krein

Kroff

et al. 2018

EPJ Web of Conferences

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Abstract. We study the dynamics of the formation of inhomogeneous chirally broken phases in the final stages of a heavy-ion collision, with particular interest on the time scales involved in the formation process. The study is conducted within the framework of a Ginzburg-Landau time evolution, driven by a free energy functional motivated by the Nambu-Jona-Lasinio model. Expansion of the medium is modeled by one-dimensional Bjorken flow and its effect on the formation of inhomogeneous condensates is investigated. We also use a free energy functional from a nonlocal Nambu-Jona-Lasinio model which predicts metastable phases that lead to long-lived inhomogeneous condensates before reaching an equilibrium phase with homogeneous condensates.

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Reaction Rates and Transport in Neutron Stars

Schmitt

Shternin

2018

Astrophysics and Space Science Library

100

122

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Understanding signals from neutron stars requires knowledge about the transport inside the star. We review the transport properties and the underlying reaction rates of dense hadronic and quark matter in the crust and the core of neutron stars and point out open problems and future directions. arXiv:1711.06520v3 [astro-ph.HE] 29 Oct 2018 65 References 66 I. INTRODUCTION A. ContextTransport describes how conserved quantities such as energy, momentum, particle number, or electric charge are transferred from one region to another. Such a transfer occurs if the system is out of equilibrium, for instance through a temperature gradient or a non-uniform chemical composition. Different theoretical methods are used to understand transport, depending on how far the system is away from its equilibrium state. If the system is close to equilibrium locally and perturbations are on large scales in space and time, hydrodynamics is a powerful technique. Further away from equilibrium other techniques are required, for example kinetic theory, which can also be used to provide the transport coefficients needed in the hydrodynamic equations. In any case, transport is determined by interactions on a microscopic level, and it is the resulting transport properties that we are concerned with in this review.Signals from neutron stars are sensitive to equilibrium properties such as the equation of state but also, to a large extent, to transport properties -here, by neutron stars we mean all objects with a radius of about 10 km and a mass of about 1-2 solar masses, including the possibilities of hybrid stars, which have a quark matter core, and pure quark stars. Therefore, understanding transport is crucial to interpret astrophysical observations, and, turning the argument around, we can use astrophysical observations to improve our understanding of transport in dense matter and thus ultimately our understanding of the microscopic interactions.Transport properties are most commonly computed from particle collisions. (Although, in strongly coupled systems, the picture of well-defined particles scattering off each other has to be taken with care.) These can be scattering processes in which energy and momentum is exchanged without changing the chemical composition of the system, or these can be flavor-changing processes from the electroweak interaction. Understanding transport thus amounts to understanding the rates of these processes, as a function of temperature and density. Electroweak processes are well understood, but large uncertainties arise if the strong interaction is involved in a reaction that contributes to transport. Therefore, approximations such as weak-coupling techniques or one-pion exchange for nucleon-nucleon collisions are being used, and efforts in current research aim at improving these approximations.In a neutron star, most of the particles involved in these processes are fermions: electrons, muons, neutrinos, neutrons, protons, hyperons, and quarks. Since the Fermi momenta of these fermions are typically much larger tha...

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Quark beta decay in the inhomogeneous chiral phase and cooling of compact stars

Cited by 18 publications

References 62 publications

Inhomogeneous chiral symmetry breaking in dense neutron-star matter

Inhomogeneous chiral symmetry breaking in dense neutron-star matter

Dynamics of inhomogeneous chiral condensates

Reaction Rates and Transport in Neutron Stars

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