Dynamical relativistic RPA calculations predict lower crust-core transition densities and pressures than thermodynamic ones across covariant energy density functionals, resulting in thinner crusts and reduced crustal moment of inertia fractions.
The Neutron Star Crust: Nuclear Physics Input
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abstract
A fully self-consistent model of the neutron star inner crust based upon models of the nucleonic equation of state at zero temperature is constructed. The results nearly match those of previous calculations of the inner crust given the same input equation of state. The extent to which the uncertainties in the symmetry energy, the compressibility, and the equation of state of low-density neutron matter affect the composition of the crust are examined. The composition and pressure of the crust is sensitive to the description of low-density neutron matter and the nuclear symmetry energy, and the latter dependence is non-monotonic, giving larger nuclei for moderate symmetry energies and smaller nuclei for more extreme symmetry energies. Future nuclear experiments may help constrain the crust and future astrophysical observations may constrain the nuclear physics input.
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nucl-th 1years
2026 1verdicts
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Thermodynamic versus Dynamical Description of the Neutron-Star Crust-Core Instability: Implications for Crustal Observables
Dynamical relativistic RPA calculations predict lower crust-core transition densities and pressures than thermodynamic ones across covariant energy density functionals, resulting in thinner crusts and reduced crustal moment of inertia fractions.