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We simulate cooling of superfluid neutron stars with nucleon cores wheredirect Urca process is forbidden. We adopt density dependent criticaltemperatures $T_{cp}(\rho)$ and $T_{cn}(\rho)$ of singlet-state proton andtriplet-state neutron pairing in a stellar core and consider a strong protonpairing (with maximum $T_{cp}^{max} \ga 5 \times 10^9$ K) and a moderateneutron pairing ($T_{cn}^{max} \sim 6 \times 10^8$ K). When the internalstellar temperature $T$ falls below $T_{cn}^{max}$, the neutrino luminosity$L_{CP}$ due to Cooper pairing of neutrons behaves $\propto T^8$, just as thatproduced by modified Urca process (in a non-superfluid star) but is higher byabout two orders of magnitude. In this case the Cooper-pairing neutrinoemission acts like an enhanced cooling agent. By tuning the density dependence$T_{cn}(\rho)$ we can explain observations of cooling isolated neutron stars inthe scenario in which direct Urca process or similar process in kaon/pioncondensed or quark matter are absent.Comment: 9 pages, 3 figures, submitted to A&

Enhanced cooling of neutron stars via Cooper-pairing neutrino emission