Cooling of neutron stars and superfluidity in their cores

Yakovlev, D. G.; Levenfish, K. P.; Shibanov, Yurii A.

doi:10.3367/ufnr.0169.199908a.0825

Cited by 66 publications

(76 citation statements)

References 182 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Superfluidity occurs when temperature falls below the critical temperature T cn . References to the numerous microscopic calculations of T cn can be found, for instance, in Yakovlev et al (1999b). The results are very sensitive to the model of nn-interaction and the many-body theory employed.…”

Section: Structure Of Neutron Starsmentioning

confidence: 95%

“…Simulations of neutron star cooling have a long history described, for instance, by Tsuruta (1998) and Yakovlev et al (1999b). However, the physical input of the models is being constantly updated as new, more accurate calculations become available.…”

Section: Neutrino Emission and Neutron Star Coolingmentioning

confidence: 99%

“…We assume further the neutron pairing of type B and the proton pairing of type A. We follow consideration of Yakovlev et al (1999b).…”

Section: Leading Reactions In Superfluid Coresmentioning

confidence: 99%

“…Almost all microscopic theories predict the appearance of neutron and proton superfluids in neutron star cores (see Yakovlev et al 1999b for references). These superfluids are believed to be produced by the nn and pp Cooper pairing due to the attractive part of the nuclear potential and can be characterized by the critical temperatures T cn and T cp .…”

Section: Structure Of Neutron Starsmentioning

confidence: 99%

“…Therefore, it is important to study the whole variety of neutrino reactions in different neutron star layers in order to analyze the cooling. Some mechanisms have been reviewed not long ago by Bisnovatyi-Kogan (1989), Pethick (1992), Itoh et al (1996), and Yakovlev et al (1999b). More references to the original and review papers are given in subsequent chapters.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

View full text Add to dashboard Cite

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.

show abstract

Section: Structure Of Neutron Starsmentioning

confidence: 95%

Section: Neutrino Emission and Neutron Star Coolingmentioning

confidence: 99%

“…We assume further the neutron pairing of type B and the proton pairing of type A. We follow consideration of Yakovlev et al (1999b).…”

Section: Leading Reactions In Superfluid Coresmentioning

confidence: 99%

Section: Structure Of Neutron Starsmentioning

confidence: 99%