Open AccessConstraints on the inner edge of neutron star crusts from relativistic nuclear energy density functionals
Author(s) -
Ch. C. Moustakidis,
Tamara Nikšić,
G. A. Lalazissis,
Dario Vretenar,
P. Ring
Publication year - 2019
Publication title -
hnps advances in nuclear physics
Language(s) - English
Resource type - Journals
eISSN - 2654-0088
pISSN - 2654-007X
DOI - 10.12681/hnps.2545
Subject(s) - isovector , neutron star , physics , symmetry (geometry) , nuclear physics , neutron , enhanced data rates for gsm evolution , energy (signal processing) , binding energy , core (optical fiber) , atomic physics , nucleon , astrophysics , quantum mechanics , geometry , telecommunications , mathematics , computer science , optics
The transition density nt and pressure Pt at the inner edge between the liquid core and the solid crust of a neutron star are analyzed using the thermodynami- cal method and the framework of relativistic nuclear energy density functionals. Starting from a functional that has been carefully adjusted to experimental binding energies of finite nuclei, and varying the density dependence of the cor- responding symmetry energy within the limits determined by isovector prop- erties of finite nuclei, we estimate the constraints on the core-crust transition density and pressure of neutron stars: 0.086 fm−3 ≤ nt < 0.090 fm−3 and 0.3 MeV fm−3 < Pt ≤ 0.76 MeV fm−3 [1].