2024 | 2023 | 2022 | 2021 | 2020 | 2019 | 2018 | 2017 | 2016 | 2015 | 2014 | 2013 | 2012 | 2011 | 2010 | 2009 | 2008

Correlation of the neutron star crust-core properties with the slope of the symmetry energy and the lead skin thickness

Authors: H. Pais, A. Sulaksono, B. K. Agrawal, C. Providência

Ref.: Phys. Rev. C 93, 045802 (2016)

Abstract: The correlations of the crust-core transition density and pressure in neutron stars with the slope of the symmetry energy and the neutron skin thickness are investigated, using different families of relativistic mean field parametrizations with constant couplings and non-linear terms mixing the $\sigma$, $\omega$ and $\rho$-meson fields. It is shown that the modification of the density dependence of the symmetry energy, involving the $\sigma$ or the $\omega$ meson, gives rise to different behaviors: the effect of the $\omega$-meson may also be reproduced within non-relativistic phenomenological models, while the effect of the $\sigma$-meson is essentially relativistic. Depending on the parametrization with $\sigma-\rho$ or $\omega-\rho$ mixing terms, different values of the slope of the symmetry energy at saturation must be considered in order to obtain a neutron matter equation of state compatible with results from chiral effective field theory. This difference leads to different pressures at the crust-core transition density. A linear correlation between the transition density and the symmetry energy slope or the neutron skin thickness of the $^{208}$Pb nucleus is obtained, only when the $\omega$-meson is used to describe the density dependence of the symmetry energy. A comparison is made between the crust-core transition properties of neutron stars obtained by three different methods, the Relativistic Random PhasApproximation (RRPA), the Vlasov equation and Thermodynamical method. \sout{The contribution of the electrons, and of the Coulomb interactionis also discussed in this study.} It is shown that the RRPA and the Vlasov methods predict similar transition densities for $pne$ $\beta$-equilibrium stellar matter.

DOI: http://dx.doi.org/10.1103/PhysRevC.93.045802

URL: arxiv.org