Cooling of neutron stars: Two types of triplet neutron superfluidity

We consider the cooling of neutron stars with superfluid cores composed of neutrons, protons, and electrons (for singlet proton pairing and triplet neutron pairing). The emphasis is on triplet neutron pairing with the component of the total moment of neutron pairs along the quantization axis |mJ| = 2. This case stands out in that it leads to power-law rather than exponential suppression of the main neutrino processes by neutron superfluidity. For the chosen critical neutron temperatures Tcn, the cooling with |mJ| = 2 proceeds either almost in the same way as the commonly considered cooling with mJ=0 or appreciably faster. The cooling with variable (over the core) critical temperatures Tcn(ρ) and Tcp(ρ) can generally be described by the cooling with some effective constant temperatures Tcn and Tcp. The hypothesis of strong neutron superfluidity with |mJ| = 2 is in conflict with the observational data on the thermal radiation from isolated neutron stars; the hypothesis of weak neutron superfluidity of any type is consistent with the observations.