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