Neutrino emission from neutron stars

Yakovlev, D. G.; Kaminker, A. D.; Gnedin, Oleg Y.; Haensel, P.

doi:10.1016/s0370-1573(00)00131-9

Cited by 549 publications

(363 citation statements)

References 187 publications

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“…For the hadronic phase, the neutrino emission processes considered in this work are the direct Urca, modified Urca and bremsstrahlung processes. A detailed review of the emissivities of such processes can be found in reference [40]. We note that the neutrino emission involving neutrons, and the neutron specific heat are exponentially suppressed as the temperature drops below the neutron superfluidity critical temperature.…”

Section: Resultsmentioning

confidence: 96%

Quark core impact on hybrid star cooling

2012

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In this paper we investigate the thermal evolution of hybrid stars, objects composed of a quark matter core, enveloped by ordinary hadronic matter. Our purpose is to investigate how important are the microscopic properties of the quark core to the thermal evolution of the star. In order to do that we use a simple MIT bag model for the quark core, and a relativistic mean field model for the hadronic envelope. By choosing different values for the microscopic parameters (bag constant, strange quark mass, strong coupling constant) we obtain hybrid stars with different quark core properties. We also consider the possibility of color superconductivity in the quark core. With this simple approach, we have found a set of microscopic parameters that lead to a good agreement with observed cooling neutron stars. Our results can be used to obtain clues regarding the properties of the quark core in hybrid stars, and can be used to refine more sophisticated models for the equation of state of quark matter.

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Section: Resultsmentioning

confidence: 96%

Quark core impact on hybrid star cooling

2012

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“…II A and (26)). This assumption makes sense because of the slowness of the electroweak reactions responsible for the chemical equilibrium [53], added to the fact that the two fluids are likely to be always very close to corotation 2 Assuming the total angular momentum to be constant during a…”

Section: B Two-fluid Hydrodynamicsmentioning

confidence: 99%

Numerical models for stationary superfluid neutron stars in general relativity with realistic equations of state

2016

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We present a numerical model for uniformly rotating superfluid neutron stars, for the first time with realistic microphysics including entrainment, in a fully general relativistic framework. We compute stationary and axisymmetric configurations of neutron stars composed of two fluids, namely superfluid neutrons and charged particles (protons and electrons), rotating with different rates around a common axis. Both fluids are coupled by entrainment, a non-dissipative interaction which in case of a non-vanishing relative velocity between the fluids, causes the fluid momenta being not aligned with the respective fluid velocities. We extend the formalism by Comer and Joynt [1] in order to calculate the equation of state (EoS) and entrainment parameters for an arbitrary relative velocity as far as superfluidity is maintained. The resulting entrainment matrix fulfills all necessary sum rules and in the limit of small relative velocity our results agree with Fermi liquid theory ones, derived to lowest order in the velocity. This formalism is applied to two new nuclear equations of state which are implemented in the numerical model. We are able to obtain precise equilibrium configurations. Resulting density profiles and moments of inertia are discussed employing both EoSs, showing the impact of entrainment and the dependence on the EoS.

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“…(13) Hence, if M 2 is known, the total neutrino emissivity from e + e − plasma can be calculated by performing appropriate integrations [13]:…”

Section: Pair Annihilation In the Standard Modelmentioning

confidence: 99%

Neutrino spectrum from the pair-annihilation process in the hot stellar plasma

2006

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An new method of calculating the energy spectrum of neutrinos and antineutrinos produced in the electron-positron annihilation processes in hot stellar plasma is presented. Detection of these neutrinos, produced copiously in the presupernova which is evolutionary advanced neutrino-cooled star, may serve in future as a trigger of pre-collapse early warning system. Also, observation of neutrinos will probe final stages of thermonuclear burning in the presupernova.The spectra obtained with the new method are compared to Monte Carlo simulations. To achieve high accuracy in the energy range of interest, determined by neutrino detector thresholds, differential cross-section for production of the antineutrino, previously unknown in an explicit form, is calculated as a function of energy in the plasma rest frame. Neutrino spectrum is obtained as a 3-dimensional integral, computed with the use of the Cuhre algorithm of at least 5% accuracy. Formulae for the mean neutrino energy and its dispersion are given as a combination of Fermi-Dirac integrals. Also, useful analytical approximations of the whole spectrum are shown.

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Neutrino emission from neutron stars

Cited by 549 publications

References 187 publications

Quark core impact on hybrid star cooling

Quark core impact on hybrid star cooling

Numerical models for stationary superfluid neutron stars in general relativity with realistic equations of state

Neutrino spectrum from the pair-annihilation process in the hot stellar plasma

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