Speaker
Description
Matching the equation of state (EoS) of pure neutron matter (PNM) with the EoS of the crust (outer and inner) of a neutron star (NS) is fundamental to understanding the properties of neutron stars, but remains a major challenge.
Our starting point here is the EoS band obtained for PNM at zero temperature and very low densities, expressed in terms of the nucleon scattering data [1], and subsequently interpolated to high-density physics by two steps (2). The first one is performed between the uncertainty band provided by (1) and the saturation density, constrained by the nuclear experimental data (symmetry energy and its slope). Then, a second interpolation is performed between this first band and the pQCD regime, where we also obtain the bands corresponding to the cases of including or not the constraints of the astrophysical observables.
In this work we incorporate to the band obtained with the previous procedure several crust models, which are connected by the coincidence of all thermodynamic quantities: pressure, energy density and baryon density. We study different matching options along the inner crust, analyzing how the matching of the crust EoS with the EoS of this band affects the NS radius, since the models describing the inner crust and the PNM EoS are not the same.
(1). J. M. Alarcón and J. A. Oller, Phys. Rev. C 107 (2023) no.4, 044319.
(2). J. M. Alarcón, E. Lope-Oter and J. A. Oller, [arXiv:2410.14776 [nucl-th]].
