Neutrino emission from neutron stars
By D. Yakovlev, M. Gusakov, A. Kaminker, A. Potekhin. 2000
341 citations recorded by the source corpus.
Abstract 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.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/31dc3a0257e7d3aa991b535ee6d5f1ba2a906416
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Citations in the corpus
- Cooling neutron star in the Cassiopeia A supernova remnant: evidence for superfluidity in the core (2010, methodology): “The protonCPF neutrino emission does not influence the cooling even if thisemission were not affected by collective effects (e.g., Yakovlev et al. 2001).”
- 2D Cooling of Magnetized Neutron Stars (2007, methodology): “(1) Yakovlev & Levenfish (1995); (2) Maxwell (1979); (3) Lattimer et al. (1991); (4) Kaminker & Yakovlev (1994); (5) Yakovlev et al. (2001); (6) Haensel et al. (1996); Kaminker et al. (1999); (7) Yakovlev et al. (1999); (8) Bezchastnov et al. (1997) The neutrino energy losses from processes that…”
- Crustal Emission and the Quiescent Spectrum of the Neutron Star in KS 1731–260 (2001, background): “Note, however, that we have neglected the effect of of neutrino emission dueto Cooper pairing of superfluid particles (see Yakovlev et al. 2001 for a review) which may reduce the value ofQcrust.”
- Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung (2019, background): “have to be considered as \identical" particles under isospin symmetry (see, e.g., discussion in Sec. 10.2-10.3 of [42]). One can also compare our sign with the corresponding sign in Eq. (161) of [43], for the case of neutrino emission. We checked that this change of sign in the exchange term wo”
- Superfluidity in nuclear systems and neutron stars (2018, background): “The cooling evolution is roughly divided into three stages (Page et al., 2013; Sedrakian, 2007; Weber, 1999; Yakovlev et al., 2001): (a) There is an initial transient stage during which the core temperature drops to about 0.1 MeV (1 MeV = 1.16× 1010 K); the subsequent thermal history of the star…”
- Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, neutral): “(24) The electron-positron pair annihilation rate into neutrinos qe−+e+→νi+νi is (e.g., Itoh et al. 1989; Yakovlev et al. 2001; Janiuk et al. 2007) qe−+e+→νi+νi = Qc 36π {(C2V,νi + C 2 A,νi )2[8(Φ1U2 + Φ2U1) −2(Φ−1U2 + Φ2U−1) + 7(Φ0U1 + Φ1U0)]} +{[5(Φ0U−1 + Φ−1U0)] +9(C2V,νi − C 2 A,νi )2[Φ0(U1 +…”
- Unified equation of state for neutron stars on a microscopic basis (2015, background): “We remind that Urca processes play an important role in the neutron star cooling (Lattimer et al. 1991; Yakovlev et al. 2001).”
- Neutron Stars—Cooling and Transport (2015, methodology): “The renormalization of the electroweak coupling is usually taken into account in an approximate manner by replacing the bare baryon masses mB with effective ones, m∗B (e.g., Yakovlev et al. 2001).”
- Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, background): “…events involving them, such as the mass, radius, moment of inertia, quadrupole deformation, pulsing frequency (Hessels et al. 2006), cooling curve (Yakovlev et al. 2001; Page et al. 2006), frequencies and damping times of various oscillating modes, spin parameter of pulsars, as well as the strain…”
- Revisiting constraints on asteroid-mass primordial black holes as dark matter candidates (2019, neutral): “[127]).”