NEUTRON AND PROTON SUPERFLUIDITY IN COOLING NEUTRON-STARS

Cooling of neutron stars is calculated when the neutrino luminosity of their cores is defined by the direct URCA process with neutrons and p rotons and is partially suppressed by the simultaneous action of the s uperfluidity of these particles. A comparison of theoretical cooling c urves with the observed thermal emission of cool isolated neutron star s poses restrictions on the critical temperatures T(cn) and T(cp) of t he neutron and proton superfluidity, respectively, which arise in cent ral parts of stars. Possible values of T(cn) and T(cp) for pulsar PSR 0656 + 14 are discussed.