Core-crust transition in neutron stars: predictivity of density developments

Дата и время публикации : 2011-02-07T11:49:21Z

Авторы публикации и институты :
Camille Ducoin (IPNO)
Jérôme Margueron (IPNO)
Constança Providência
Isaac Vidaña

Ссылка на журнал-издание: Phys.Rev.C83:045810,2011
Коментарии к cтатье: Ссылка на журнал-издание не найдена
Первичная категория: nucl-th

Все категории : nucl-th, astro-ph.SR

Краткий обзор статьи: The possibility to draw links between the isospin properties of nuclei and the structure of compact stars is a stimulating perspective. In order to pursue this objective on a sound basis, the correlations from which such links can be deduced have to be carefully checked against model dependence. Using a variety of nuclear effective models and a microscopic approach, we study the relation between the predictions of a given model and those of a Taylor density development of the corresponding equation of state: this establishes to what extent a limited set of phenomenological constraints can determine the core-crust transition properties. From a correlation analysis we show that a) the transition density $rho_t$ is mainly correlated with the symmetry energy slope $L$, b) the proton fraction $Y_{p,t}$ with the symmetry energy and symmetry energy slope $(J,L)$ defined at saturation density, or, even better, with the same quantities defined at $rho=0.1$ fm$^{-3}$, and c) the transition pressure $P_t$ with the symmetry energy slope and curvature $(J,K_{rm sym})$ defined at $rho=0.1$ fm$^{-3}$.

Category: Physics