Coherent neutrino radiation in supernovae at two loops

This review describes the properties of hadronic phases of dense matter in compact stars. The theory is developed within the method of real-time Green's functions and is applied to study of baryonic matter at and above the saturation density. The non-relativistic and covariant theories based on continuum Green's functions and the T -matrix and related approximations to the selfenergies are reviewed. The effects of symmetry energy, onset of hyperons and meson condensation on the properties of stellar configurations are demonstrated on specific examples. Neutrino interactions with baryonic matter are introduced within a kinetic theory. We concentrate on the classification, analysis and first principle derivation of neutrino radiation processes from unpaired and superfluid hadronic phases. We then demonstrate how neutrino radiation rates from various microscopic processes affect the macroscopic cooling of neutron stars and how the observed X-ray fluxes from pulsars constrain the properties of dense hadronic matter. Contents IntroductionNeutron stars are born in a gravitational collapse of luminous stars whose core mass exceeds the Chandrasekhar limit for a self-gravitating body supported by degeneracy pressure of electron gas [1]. Being the densest observable bodies in our universe they open a window on the physics of matter under extreme conditions of high densities, pressures and strong electromagnetic and gravitational fields. Most of the known pulsars are isolated objects which emit radio-waves at frequencies 10 8 − 10 10 Hz, which are pulsed at the rotation frequency of the star. Young objects, like the pulsar in the Crab nebula, are also observed through X-rays that are emitted from their surface as the star radiates away its thermal energy. Relativistic magnetospheres of young pulsars emit detectable non-thermal optical and gamma radiation; they could be sources of high-energy elementary particles. Neutron stars in the binaries are powered by the energy of matter accreted from companion star.The radio observations of pulsars stretch back to 1967 when the first pulsar was discovered. Since then, the observational pulsar astronomy has been extremely important to the fundamental physics and 2 astrophysics, which is evidenced by two Nobel awards, one for the discovery of pulsars (Hewish 1974) [2], the other for the discovery of the first neutron star -neutron star binary pulsar (Hulse and Taylor, 1993) [3] whose orbital decay confirmed the gravitational radiation in full agreement with Einstein's General Theory of Relativity. The measurements of neutron star (NS) masses in binaries provide one of the most stringent constraint on properties of the superdense matter. The timing observations of the millisecond pulsars set an upper limit on the angular momentum that can be accommodated by a stable NS -a limit that can potentially constrains the properties of dense matter. Noise and rotational anomalies that are superimposed on the otherwise highly stable rotation of these objects provide a clue to the ...

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“…The collision integrals for neutrinos and anti-neutrinos can be combined if one uses the identities Π [191,198,202] …”

Section: Neutral Current Processes (Bremsstrahlung)mentioning

confidence: 99%

The physics of dense hadronic matter and compact stars

Sedrakian

2007

Progress in Particle and Nuclear Physics

126

109

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“…This is the equivalent for scattering to the Landau-Migdal-Pomeranchuk effect studied in the case of neutrino Bremsstrahlung by [23,24,29].…”

Section: Rpa Correctionsmentioning

confidence: 99%

“…These have been studied separately from RPA corrections by several autors (see eg. [19,20,23,24]). The calculated correction factors to the neutrino opacities are large, especially in the low density regime.…”

Section: Summary and Perspectivesmentioning

confidence: 99%

“…While early calculations only were taking into account the nucleon mass reduction in the medium, important progress has been realized since then in order to include Hartree-Fock [10], random phase approximation (RPA) [11,12,13,14,15,16,17] or ladder [18,19,20,21,22,23,24] correlations. It is generally found that the neutrino opacities are suppressed by medium effects, if however no collective mode is excited [16].…”

Section: Introductionmentioning

confidence: 99%

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Neutrino-nucleon scattering rate in proto-neutron star matter

Mornas

Perez

2002

Eur Phys J A

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We present a calculation of the neutrino-nucleon scattering cross section which takes into account the nuclear correlations in the relativistic random phase approximation. Our approach is based on a quantum hadrodynamics model with exchange of σ, ω, π, ρ and δ mesons. In view of applications to neutrino transport in the final stages of supernova explosion and protoneutron star cooling, we study the evolution of the neutrino mean free path as a function of density, proton-neutron asymmetry and temperature. Special attention was paid to the issues of renormalization of the Dirac sea, residual interactions in the tensor channel and meson mixing. It is found that RPA corrections, with respect to the mean field approximation, amount to only 10% to 15% at high density.

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“…One approach to estimate the emission rate relies on linear response theory where emission, absorption, and scattering of neutrinos, axions and other particles depend only on a few "form factors" of the medium, i.e., the dynamical structure functions [73,[78][79][80][81][82][83][84][85][86]. This approach is perturbative to lowest order in the weak interaction between neutrinos (or axions) and nucleons, whereas the interactions among the medium constituents are lumped into the structure functions.…”

Section: Axion Emission From a Nuclear Mediummentioning

confidence: 99%

Astrophysical Axion Bounds

Raffelt

Lecture Notes in Physics

552

688

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Summary. Axion emission by hot and dense plasmas is a new energy-loss channel for stars. Observational consequences include a modification of the solar sound-speed profile, an increase of the solar neutrino flux, a reduction of the helium-burning lifetime of globular-cluster stars, accelerated white-dwarf cooling, and a reduction of the supernova SN 1987A neutrino burst duration. We review and update these arguments and summarize the resulting axion constraints.

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Coherent neutrino radiation in supernovae at two loops

Cited by 35 publications

References 22 publications

The physics of dense hadronic matter and compact stars

The physics of dense hadronic matter and compact stars

Neutrino-nucleon scattering rate in proto-neutron star matter

Astrophysical Axion Bounds

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