Relativistic Correction on Neutrino Emission from Neutron Stars in Various Parameter Sets

Ding, Wen-Bo; Qi, Zhan-Qiang; Hou, Jia-Wei; Mi, Geng; Bao, Tmurbagan; Zi, Yu; Liu, Guangzhou; Zhao, En-Guang

doi:10.1088/0253-6102/66/4/474

Cited by 3 publications

(3 citation statements)

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“…Other works use the relativistic formalism, but assume the nuclear matter is strongly degenerate (using the Fermi surface approximation, described below), and thus their results have a sharp direct Urca threshold density [15][16][17]. Ref.…”

Section: Introductionmentioning

confidence: 99%

Beta Equilibrium under Neutron Star Merger Conditions

et al. 2021

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We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1MeV<T≲5MeV. We improve on previous work using a consistent description of nuclear matter based on the IUF and SFHo relativistic mean field models. This includes using relativistic dispersion relations for the nucleons, which we show is essential in these models. We find that the nonzero-temperature correction can be of order 10 to 20 MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of 10 or more if it is neglected.

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Section: Introductionmentioning

confidence: 99%

Beta Equilibrium under Neutron Star Merger Conditions

et al. 2021

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Section: Introductionmentioning

confidence: 99%

Beta equilibrium under neutron star merger conditions

Alford,

Haber,

Harris

et al. 2021

Preprint

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We calculate the isospin chemical potential that is required for beta equilibrium in nuclear matter under neutron star merger conditions, in the temperature range 1 MeV < T 5 MeV. We improve on previous work by using a consistent description of nuclear matter based on the IUF and SFHo relativistic mean field models. This includes using relativistic dispersion relations for the nucleons, which we show is essential in these models.We find that the isospin chemical potential can be of order 10 to 20 MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of 10 or more if it is neglected.

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“…For modifications of the direct Urca rate in various parameterizations in the framework of relativistic mean field theories see also Ref. [262].…”

Section: Neutrino Emission Of Nuclear Mattermentioning

confidence: 99%

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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Relativistic Correction on Neutrino Emission from Neutron Stars in Various Parameter Sets

Cited by 3 publications

References 20 publications

Beta Equilibrium under Neutron Star Merger Conditions

Beta Equilibrium under Neutron Star Merger Conditions

Beta equilibrium under neutron star merger conditions

Reaction Rates and Transport in Neutron Stars

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