A Brief, Biased View of Neutron Star Cooling

ABSTRACT This is a concise and non‐technical review of topics related to neutron star (NS) cooling, for both young NSs and NSs in low‐mass x‐ray binaries. Neutrino emission from the NS core drives cooling rates, via different processes including Urca processes and pair breaking and formation at the neutron superfluid critical temperature. Key insights have been given by the temperatures of the coldest NSs, by the rapid (questioned) cooling of the Cas A NS, and by measuring the cooling of transient NS x‐ray binaries after accretion episodes.