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X-ray observations of the neutron star in the Cas A supernova remnant overthe past decade suggest the star is undergoing a rapid drop in surfacetemperature of $\approx$ $2-5.5\%$. One explanation suggests the rapid coolingis triggered by the onset of neutron superfluidity in the core of the star,causing enhanced neutrino emission from neutron Cooper pair breaking andformation (PBF). Using consistent neutron star crust and core equations ofstate (EOSs) and compositions, we explore the sensitivity of thisinterpretation to the density dependence of the symmetry energy $L$ of the EOSused, and to the presence of enhanced neutrino cooling in the bubble phases ofcrustal "nuclear pasta". Modeling cooling over a conservative range of neutronstar masses and envelope compositions, we find $L\lesssim70$ MeV, competitivewith terrestrial experimental constraints and other astrophysical observations.For masses near the most likely mass of $M\gtrsim 1.65 M_{\odot}$, theconstraint becomes more restrictive $35\lesssim L\lesssim 55$ MeV. Theinclusion of the bubble cooling processes decreases the cooling rate of thestar during the PBF phase, matching the observed rate only when $L\lesssim45$MeV, taking all masses into consideration, corresponding to neutron star radii$\lesssim 11$km.

The cooling of the Cassiopeia A neutron star as a probe of the nuclear symmetry energy and nuclear pasta