Neutrino pair bremsstrahlung by nucleons in neutron-star matter

Flowers, E. G.; Sutherland, P. G.; Bond, J. R.

doi:10.1103/physrevd.12.315

Cited by 38 publications

(34 citation statements)

References 15 publications

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“…(49), while S AB and S BC are defined by Eqs. (51), (52) and (55). These equations are sufficient for practical use.…”

Section: Neutrino Synchrotron Emission By Degenerate Electrons (A) Qumentioning

confidence: 95%

“…The modified Urca processes were introduced in the context of neutron star cooling by Chiu and Salpeter (1964). They were studied by Bahcall and Wolf (1965a, b), Flowers et al (1975), Friman and Maxwell (1979), as well as by Maxwell (1987). The most detailed paper seems to be that by Friman and Maxwell, which however neglected the proton branch.…”

Section: Modified Urca Process (A) Emissivitymentioning

confidence: 99%

“…According to Nadyozhin and Chechetkin (1969), the Urca processes produce highly efficient neutrino emission in a hot plasma of the temperature T > ∼ 10 10 K in the density range from about 10 5 to 10 12 g cm −3 . For lower T < ∼ 10 10 K, we are interested in, the density dependence of the neutrino emissivity has maximum at ρ ∼ 10 9 g cm −3 produced by beta decays of the 55 Cr and 53 V nuclei with high energy release (∼ 2.5 MeV per beta-decay). The decrease of the emissivity at higher densities is mainly explained by transformation of 55 Cr and 53 V into less active 56 Cr and neutrons.…”

Section: Beta Processes (A) General Remarksmentioning

confidence: 99%

“…For lower T < ∼ 10 10 K, we are interested in, the density dependence of the neutrino emissivity has maximum at ρ ∼ 10 9 g cm −3 produced by beta decays of the 55 Cr and 53 V nuclei with high energy release (∼ 2.5 MeV per beta-decay). The decrease of the emissivity at higher densities is mainly explained by transformation of 55 Cr and 53 V into less active 56 Cr and neutrons. In addition, the electron reaction rates are reduced by the Pauli principle and the positron reaction rates are reduced by the decrease of the positron number density because of growing electron degeneracy.…”

Section: Beta Processes (A) General Remarksmentioning

confidence: 99%

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Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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“…(49), while S AB and S BC are defined by Eqs. (51), (52) and (55). These equations are sufficient for practical use.…”

Section: Neutrino Synchrotron Emission By Degenerate Electrons (A) Qumentioning

confidence: 95%

Section: Modified Urca Process (A) Emissivitymentioning

confidence: 99%

Section: Beta Processes (A) General Remarksmentioning

confidence: 99%

Section: Beta Processes (A) General Remarksmentioning

confidence: 99%

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Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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“…Early studies of the bremsstrahlung at the quasiparticle level modelled the strong force using the T -matrix interaction [3], the free-space one-boson exchange interaction [4] and their in-medium modifications [5] supplemented with a hard core modelled in the spirit of the Fermi-liquid theory. The explicit use of the tensor interaction turned out to be crucial as there are significant cancellations among different diagrams, and the surviving contribution is due to a non-trivial contraction between the operator structures of the weak and strong interactions (tensor force) [4].…”

Section: Introductionmentioning

confidence: 99%

Coherent neutrino radiation in supernovae at two loops

Sedrakian

Dieperink

2000

Phys. Rev. D

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We develop a neutrino transport theory, in terms of the real-time nonequilibrium Green's functions, which is applicable to physical conditions arbitrary far from thermal equilibrium. We compute the coherent neutrino radiation in cores of supernovae by evaluating the two-particle-two-hole (2p-2h) polarization function with dressed propagators. The propagator dressing is carried out in the particle-particle channel to all orders in the interaction. We show that at two loops there are two distinct sources of coherence effects in the bremsstrahlung. One is the generically off-shell intermediate state propagation, which leads to the Landau-Pomeranchuk-Migdal type suppression of radiation. We extend previous perturbative results, obtained in the leading order in quasiparticle width, by deriving the exact non-perturbative expression. A new contribution due to off-shell finial/initial baryon states is treated in the leading order in the quasiparticle width. The latter contribution corresponds to processes of higher order than second order in the virial expansion in the number of quasiparticles. At 2p-2h level, the time component of the polarization tensor for the vector transitions vanishes identically in the soft neutrino approximation. Vector current thereby is conserved. The contraction of the neutral axial vector current with tensor interaction among the baryons leads to a non-vanishing contribution to the bremsstrahlung rate. These rates are evaluated numerically for finite temperature pure neutron

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References

1983

Black Holes, White Dwarfs, and Neutron Stars

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Neutrino pair bremsstrahlung by nucleons in neutron-star matter

Cited by 38 publications

References 15 publications

Neutrino emission from neutron stars

Neutrino emission from neutron stars

Coherent neutrino radiation in supernovae at two loops

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