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Neutron stars cooling after sustained accretion outbursts provide uniqueinformation about the neutron star crust and underlying dense matter.Comparisons between astronomical observations of these cooling transients andmodel calculations of neutron star crust cooling have frequently been used toconstrain neutron star properties such as the mass, radius, crust composition,and presence of nuclear pasta. These calculations often use a fixed pressure atwhich the crust-core transition happens, though this quantity depends on thedense matter equation of state. We demonstrate that varying the crust-coretransition pressure in a manner consistent with adopting various equations ofstate results in modest changes to the crust cooling light curve. Thisvalidates the approach adopted in most crust cooling studies to date, where theneutron star mass and radius are varied while leaving the crust-core transitionpressure constant.

Crust Cooling Models are Insensitive to the Crust-Core Transition Pressure for Realistic Equations of State