Neutrino pair emission from finite-temperature neutron superfluid and the cooling of young neutron stars

Journal Article · Thu Apr 15 00:00:00 EST 1976 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/154308· OSTI ID:7272752

Flowers, E; Ruderman, M; Sutherland, P

The neutrons inside neutron stars are almost certainly superfluid below a critical temperature T/subc/approx.10/sup 10/ K. Below T/subc/, pairs of excited neutron quasiparticles may recombine, resulting, if weak neutral currents exist, in the emission of neutrino-antineutrino pairs. We calculate the emissivity associated with this process and compare it with other neutrino emissivities. For neutron star interior temperatures in the range 10/sup 9/-10/sup 10/ K the recombination emissivity can dominate all others. (AIP)

• Research Organization: Department of Physics, New York University
• OSTI ID: 7272752
• Journal Information: Astrophys. J.; (United States), Vol. 205:2
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
NEUTRON STARS
COOLING
SUPERFLUIDITY
ANTINEUTRINOS
BREMSSTRAHLUNG
EMISSION
EMISSIVITY
NEUTRINOS
NEUTRONS
NUCLEAR REACTIONS
RECOMBINATION
TEMPERATURE DEPENDENCE
ANTILEPTONS
ANTIMATTER
ANTIPARTICLES
BARYONS
ELECTROMAGNETIC RADIATION
ELEMENTARY PARTICLES
FERMIONS
HADRONS
LEPTONS
MASSLESS PARTICLES
NUCLEONS
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
RADIATIONS
STARS
SURFACE PROPERTIES
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources