Core-crust transition in neutron stars: Predictivity of density developments
- CFC, Department of Physics, University of Coimbra, PT-3004-516, Coimbra (Portugal)
- Institut de Physique Nucleaire, Universite Paris-Sud, IN2P3-CNRS, FR-91406 Orsay Cedex (France)
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}{sub t} is mainly correlated with the symmetry energy slope L, (b) the proton fraction Y{sub 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{sup -3}, and (c) the transition pressure P{sub t} with the symmetry energy slope and curvature (L,K{sub sym}) defined at {rho}=0.1 fm{sup -3}.
- OSTI ID:
- 21499636
- Journal Information:
- Physical Review. C, Nuclear Physics, Vol. 83, Issue 4; Other Information: DOI: 10.1103/PhysRevC.83.045810; (c) 2011 American Institute of Physics; ISSN 0556-2813
- Country of Publication:
- United States
- Language:
- English
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