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

2016 ◽  
Vol 93 (4) ◽  
Author(s):  
H. Pais ◽  
A. Sulaksono ◽  
B. K. Agrawal ◽  
C. Providência
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Skin Thickness ◽  
Neutron Star Crust

scholarly journals Symmetry Energy, Neutron Star Crust and Neutron Skin Thickness

2010 ◽  
Vol 50 (1-4) ◽  
pp. 327-329
Author(s):  
Isaac Vidaña ◽  
Constança Providência ◽  
Artur Polls ◽  
Arnau Rios
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Neutron Star Crust ◽  
Neutron Skin Thickness ◽  
Energy Neutron

scholarly journals The Equation of State of Nuclear Matter: From Finite Nuclei to Neutron Stars

Universe ◽  
2020 ◽  
Vol 6 (8) ◽  
pp. 119 ◽  
Author(s):  
G. Fiorella Burgio ◽  
Isaac Vidaña
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Quantum Monte Carlo ◽  
Equations Of State ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Large Set ◽  
Solar Mass ◽  
Atomic Nuclei ◽  
Neutron Skin Thickness

Background. We investigate possible correlations between neutron star observables and properties of atomic nuclei. In particular, we explore how the tidal deformability of a 1.4 solar mass neutron star, M1.4, and the neutron-skin thickness of 48Ca and 208Pb are related to the stellar radius and the stiffness of the symmetry energy. Methods. We examine a large set of nuclear equations of state based on phenomenological models (Skyrme, NLWM, DDM) and ab initio theoretical methods (BBG, Dirac–Brueckner, Variational, Quantum Monte Carlo). Results: We find strong correlations between tidal deformability and NS radius, whereas a weaker correlation does exist with the stiffness of the symmetry energy. Regarding the neutron-skin thickness, weak correlations appear both with the stiffness of the symmetry energy, and the radius of a M1.4. Our results show that whereas the considered EoS are compatible with the largest masses observed up to now, only five microscopic models and four Skyrme forces are simultaneously compatible with the present constraints on L and the PREX experimental data on the 208Pb neutron-skin thickness. We find that all the NLWM and DDM models and the majority of the Skyrme forces are excluded by these two experimental constraints, and that the analysis of the data collected by the NICER mission excludes most of the NLWM considered. Conclusion. The tidal deformability of a M1.4 and the neutron-skin thickness of atomic nuclei show some degree of correlation with nuclear and astrophysical observables, which however depends on the ensemble of adopted EoS.

scholarly journals Structure of Strange Quark Matter and Neutron Stars

2004 ◽  
Vol 218 ◽  
pp. 289-296
Author(s):  
James M. Lattimer
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Nuclear Physics ◽  
Laboratory Experiments ◽  
Nuclear Astrophysics ◽  
Analytic Solutions ◽  
Strong Interactions ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Global Features

The properties of neutron and strange matter stars are discussed from global and observational perspectives. The global features, i.e., the mass-radius relation, the moment of inertia, and the binding energy, of these objects can be understood by examination of the few known relevant analytic solutions to Einstein's equations. A close connection exists between neutron star radii and the density dependence of the isospin dependence of strong interactions, i.e., the nuclear symmetry energy. Interestingly, a similar relation has been found to exist between the symmetry energy and the neutron skin thickness of neutron-rich nuclei, the object of a new generation of laboratory experiments, although these are 1018 times smaller. Recent observations of neutron star masses and radiation radii are summarized. The status of these observations as predictors of nuclear force properties is examined. The combination of observations, laboratory experiments, and theory is an extremely powerful tool for both nuclear physics and nuclear astrophysics.

scholarly journals Constraints on the symmetry energy from observational probes of the neutron star crust

2014 ◽  
Vol 50 (2) ◽  
Author(s):  
William G. Newton ◽  
Joshua Hooker ◽  
Michael Gearheart ◽  
Kyleah Murphy ◽  
De-Hua Wen ◽  
...  
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Neutron Star Crust

The symmetry energy: Predictions and constraints

2017 ◽  
Vol 32 (30) ◽  
pp. 1730027 ◽  
Author(s):  
Francesca Sammarruca
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Heavy Ion ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Nuclear Forces ◽  
Neutron Skin Thickness ◽  
Density Derivative ◽  
Proper Consideration ◽  
Future Plans

After recalling basic phenomenological features of isospin asymmetric nuclear matter, we review predictions for the interaction part of the symmetry energy obtained from different microscopic approaches. The predictions are compared to updated constraints extracted from heavy-ion (HI) reaction observables of a recent GSI experiment. The discussion is extended to the neutron skin thickness in [Formula: see text] and its relation to the density derivative of the symmetry energy. We underline the importance of giving proper consideration to the theoretical uncertainties of microscopic predictions in order to guide phenomenological analyses. In the end, we report briefly on preliminary neutron star calculations based on chiral nuclear forces and outline future plans.

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