scholarly journals Role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a neutron star with unified equations of state

2019 ◽  
Vol 100 (3) ◽  
Author(s):  
L. Perot ◽  
N. Chamel ◽  
A. Sourie
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Equations Of State ◽  
Neutron Matter

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 The equation of state of neutron matter, symmetry energy and neutron star structure

2014 ◽  
Vol 50 (2) ◽  
Author(s):  
S. Gandolfi ◽  
J. Carlson ◽  
S. Reddy ◽  
A. W. Steiner ◽  
R. B. Wiringa
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Symmetry Energy ◽  
Neutron Matter ◽  
Star Structure

scholarly journals Hyperons in hot dense matter: what do the constraints tell us for equation of state?

2018 ◽  
Vol 35 ◽  
Author(s):  
M. Fortin ◽  
M. Oertel ◽  
C. Providência
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Symmetry Energy ◽  
Nuclear Physics ◽  
Equations Of State ◽  
Dense Matter ◽  
Baryon Octet ◽  
Thermodynamic Quantities ◽  
Binary Neutron Star ◽  
Hot Matter

AbstractFor core-collapse and neutron star merger simulations, it is important to have adequate equations of state which describe dense and hot matter as realistically as possible. We present two newly constructed equations of state including the entire baryon octet, compatible with the main constraints coming from nuclear physics, both experimental and theoretical. One of the equations of state describes cold β-equilibrated neutron stars with a maximum mass of 2 Msun. Results obtained with the new equations of state are compared with the ones of DD2Y, the only existing equation of state containing the baryon octet and satisfying the above constraints. The main difference between our new equations of state and DD2Y is the harder symmetry energy of the latter. We show that the density dependence of the symmetry energy has a direct influence on the amount of strangeness inside hot and dense matter and, consequently, on thermodynamic quantities. We expect that these differences affect the evolution of a proto-neutron star or binary neutron star mergers. We propose also several parameterisations based on the DD2 and SFHo models calibrated to Lambda hypernuclei that satisfy the different constraints.

scholarly journals Nuclear symmetry energy effects on neutron stars properties

2020 ◽  
Vol 15 ◽  
pp. 128
Author(s):  
Ch. C. Moustakidis ◽  
V. P. Psonis ◽  
S. E. Massen
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Systematic Study ◽  
Symmetry Energy ◽  
Potential Model ◽  
Equations Of State ◽  
Baryon Density ◽  
Nuclear Symmetry Energy ◽  
Global Properties ◽  
Potential Part

We construct a class of nuclear equations of state based on a schematic potential model, that originates from the work of Prakash et. al. [1], which reproduce the results of most microscopic calculations. The equations of state are used as input for solving the Tolman- Oppenheimer-Volkov equations for corresponding neutron stars. The potential part contribution of the symmetry energy to the total energy is parameterized in a generalized form both for low and high values of the baryon density. The obtained nuclear equations of state are applied for the systematic study of the global properties of a neutron star (masses, radii and composition). We also address on the problem of the existence of correlation between the pressure near the saturation density and the radius.

scholarly journals Nuclear equation of state constraints from tidal deformability of neutron stars

2019 ◽  
Vol 21 ◽  
pp. 44
Author(s):  
Ch. C. Moustakidis
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Symmetry Energy ◽  
State Constraints ◽  
Equations Of State ◽  
Recent Observation ◽  
Nuclear Symmetry Energy ◽  
Nuclear Equation Of State ◽  
Theoretical Predictions

We study the effect of nuclear equation of state on the tidal polarizability of neutron stars. The predicted equations of state for the β-stable nuclear matter are parameterized by varying the slope L of the symmetry energy at saturation density on the interval 65 MeV≤L≤115 MeV. The effects of the density dependence of the nuclear symmetry energy on the neutron star tidal polarizability are presented and analyzed. A comparison of theoretical predictions with the recent observation predictions is also performed and analyzed.

scholarly journals Erratum: Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. I. Role of symmetry energy

2019 ◽  
Vol 486 (1) ◽  
pp. 768-768 ◽  
Author(s):  
J M Pearson ◽  
N Chamel ◽  
A Y Potekhin ◽  
A F Fantina ◽  
C Ducoin ◽  
...  
Keyword(s):  
Neutron Stars ◽  
Symmetry Energy ◽  
Equations Of State

scholarly journals NUCLEAR SYMMETRY ENERGY EFFECTS ON NEUTRON STARS PROPERTIES

2007 ◽  
Vol 22 (17) ◽  
pp. 1233-1253 ◽  
Author(s):  
V. P. PSONIS ◽  
CH. C. MOUSTAKIDIS ◽  
S. E. MASSEN
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Symmetry Energy ◽  
Linear Relation ◽  
Equations Of State ◽  
Baryon Density ◽  
Saturation Density ◽  
Global Properties ◽  
Dense Nuclear Matter ◽  
Potential Part

We construct a class of nuclear equations of state based on a schematic potential model, that originates from the work of Prakash et al.,1 which reproduce the results of most microscopic calculations. The equations of state are used as input for solving the Tolman–Oppenheimer–Volkov equations for the corresponding neutron stars. The potential part contribution of the symmetry energy to the total energy is parametrized in a generalized form both for low and high values of the baryon density. Special attention is devoted to the construction of the symmetry energy in order to reproduce the results of most microscopic calculations of dense nuclear matter. The obtained nuclear equations of state are applied for the systematic study of the global properties of a neutron star (masses, radii and composition). The calculated masses and radii of the neutron stars are plotted as a function of the potential part parameters of the symmetry energy. A linear relation between these parameters, the radius and the maximum mass of the neutron star is obtained. In addition, a linear relation between the radius and the derivative of the symmetry energy near the saturation density is found. We also address the problem of the existence of correlation between the pressure near the saturation density and the radius.

scholarly journals Role of the symmetry energy on the structure of neutron stars with unified equations of state

2019 ◽  
Author(s):  
Nicolas Chamel ◽  
John Michael Pearson ◽  
Alexander Y. Potekhin ◽  
Anthea F. Fantina ◽  
Camille Ducoin ◽  
...  
Keyword(s):  
Neutron Stars ◽  
Symmetry Energy ◽  
Equations Of State
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