Abstract
This paper presents a method for estimating the pressure variance at the inner edge of a neutron star crust. The obtained results quantify uncertainty in the estimation of pressure at the core-crust interface, implying that they depend on the selected equation of state and the neutron star's mass distribution function. The quality of the transition pressure determination depends on the neutron star's mass, with a significant decrease in accuracy for configurations with masses close to $2\mathrm{M}\ensuremath{\bigodot}$. The method used makes it possible to control the theoretical part of the core-crust pressure dispersion in determining the observational quantities.
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