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The study of how neutron stars cool over time can provide invaluable insightsinto fundamental physics such as the nuclear equation of state andsuperconductivity and superfluidity. A critical relation in neutron starcooling is the one between observed surface temperature and interiortemperature. This relation is determined by the composition of the neutron starenvelope and can be influenced by the process of diffusive nuclear burning(DNB). We calculate models of envelopes that include DNB and find that DNB canlead to a rapidly changing envelope composition which can be relevant forunderstanding the long-term cooling behavior of neutron stars. We also reporton analysis of the latest temperature measurements of the young neutron star inthe Cassiopeia A supernova remnant. The 13 Chandra observations over 18 yearsshow that the neutron star's temperature is decreasing at a rate of 2-3 percentper decade, and this rapid cooling can be explained by the presence of a protonsuperconductor and neutron superfluid in the core of the star.

Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning