Neutrino energy loss in stellar interiors. III - Pair, photo-, plasma, and bremsstrahlung processes

Itoh, Naoki; Adachi, Tomoo; Nakagawa, Masayuki; Kohyama, Yasuharu; Munakata, Hiroharu

doi:10.1086/167301

Cited by 186 publications

(172 citation statements)

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“…Dicus (1972), Munakata et al (1985), Schinder et al (1987), and Itoh et al (1989Itoh et al ( , 1996 derived the fits which do not differ strongly from one another and reproduce Q pair sufficiently accurately at those values of T and ρ where the pair annihilation mechanism is most efficient. However, their fit formulae are chosen in such a way that they do not reproduce the asymptotes of Q pair .…”

Section: Annihilation Of Electron-positron Pairs (A) Emissivitymentioning

confidence: 85%

“…2.5). The emissivity of the latter process is taken from Itoh et al (1989Itoh et al ( , 1996. Finally, 'brems' is the neutrino bremsstrahlung due to the electron-nucleus scattering.…”

Section: (C) Illustrative Figuresmentioning

confidence: 99%

“…Beaudet et al (1967) considered also different limiting behavior of Q pair . Subsequently, the process was studied by a number of authors (e.g., Dicus 1972, Munakata et al 1985, Schinder et al 1987, Blinnikov and Rudzskii 1989, Itoh et al 1989, 1996. We discuss some of the results below.…”

Section: Annihilation Of Electron-positron Pairs (A) Emissivitymentioning

confidence: 99%

“…Photoneutrino emission was proposed by Ritus (1961) and Chiu and Stabler (1961). The emissivity was calculated by Beaudet et al (1967), Dicus (1972), Munakata et al (1985), Schinder et al (1987), and Itoh et al (1989Itoh et al ( , 1996. In particular, Itoh et al (1989) presented extensive tables of the photoneutrino emissivity for ρ < ∼ 10 10 g cm −3 .…”

Section: Other Electron-photon Neutrino Processesmentioning

confidence: 99%

“…The emissivity was calculated by Beaudet et al (1967), Dicus (1972), Munakata et al (1985), Schinder et al (1987), and Itoh et al (1989Itoh et al ( , 1996. In particular, Itoh et al (1989) presented extensive tables of the photoneutrino emissivity for ρ < ∼ 10 10 g cm −3 . Many authors proposed analytic fits; the most recent ones were given by Itoh et al (1989Itoh et al ( , 1996.…”

Section: Other Electron-photon Neutrino Processesmentioning

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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Section: Annihilation Of Electron-positron Pairs (A) Emissivitymentioning

confidence: 85%

“…2.5). The emissivity of the latter process is taken from Itoh et al (1989Itoh et al ( , 1996. Finally, 'brems' is the neutrino bremsstrahlung due to the electron-nucleus scattering.…”

Section: (C) Illustrative Figuresmentioning

confidence: 99%