scholarly journals Hyperons and nuclear symmetry energy in neutron star matter

2011 ◽  
Vol 84 (3) ◽  
Author(s):  
Chung-Yeol Ryu ◽  
Chang Ho Hyun ◽  
Chang-Hwan Lee
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Nuclear Symmetry Energy ◽  
Neutron Star Matter

scholarly journals Equation of state of neutron star matter, and the nuclear symmetry energy

2011 ◽  
Vol 83 (6) ◽  
Author(s):  
Doan Thi Loan ◽  
Ngo Hai Tan ◽  
Dao T. Khoa ◽  
Jerome Margueron
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Symmetry Energy ◽  
Nuclear Symmetry Energy ◽  
Neutron Star Matter

scholarly journals Studying the parameters of the extended σ-ω model for neutron star matter

2020 ◽  
Vol 229 (22-23) ◽  
pp. 3615-3628
Author(s):  
David Alvarez-Castillo ◽  
Alexander Ayriyan ◽  
Gergely Gábor Barnaföldi ◽  
Hovik Grigorian ◽  
Péter Pósfay
Keyword(s):  
Neutron Star ◽  
Bayesian Analysis ◽  
Neutron Stars ◽  
Symmetry Energy ◽  
State Of The Art ◽  
Saturation Density ◽  
Mass Limit ◽  
Neutron Star Matter

AbstractIn this work we study the parameters of the extended σ-ω model for neutron star matter by a Bayesian analysis of state-of-the-art multi-messenger astronomy observations, namely mass, radius and tidal deformabilities. We have considered three parameters of the model, the Landau mass mL, the nuclear compressibility K0, and the value of the symmetry energy S0, all at saturation density n0. As a result, we are able to estimate the best values of the Landau mass of mL ≈ 0.73 GeV, whereas the values of K0 and S0 fall within already known empirical values. Furthermore, for neutron stars we find the most probable value of 13 km < R1.4 < 13.5 km and the upper mass limit of Mmax ≈ 2.2 M⊙.

scholarly journals A Modern View of the Equation of State in Nuclear and Neutron Star Matter

Symmetry ◽  
2021 ◽  
Vol 13 (3) ◽  
pp. 400
Author(s):  
G. Fiorella Burgio ◽  
Hans-Josef Schulze ◽  
Isaac Vidaña ◽  
Jin-Biao Wei
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Symmetry Energy ◽  
Quantum Monte Carlo ◽  
Mean Field ◽  
Nuclear Symmetry Energy ◽  
Relativistic Mean Field ◽  
Monte Carlo Techniques ◽  
Nuclear Incompressibility

Background: We analyze several constraints on the nuclear equation of state (EOS) currently available from neutron star (NS) observations and laboratory experiments and study the existence of possible correlations among properties of nuclear matter at saturation density with NS observables. Methods: We use a set of different models that include several phenomenological EOSs based on Skyrme and relativistic mean field models as well as microscopic calculations based on different many-body approaches, i.e., the (Dirac–)Brueckner–Hartree–Fock theories, Quantum Monte Carlo techniques, and the variational method. Results: We find that almost all the models considered are compatible with the laboratory constraints of the nuclear matter properties as well as with the largest NS mass observed up to now, 2.14−0.09+0.10M⊙ for the object PSR J0740+6620, and with the upper limit of the maximum mass of about 2.3–2.5M⊙ deduced from the analysis of the GW170817 NS merger event. Conclusion: Our study shows that whereas no correlation exists between the tidal deformability and the value of the nuclear symmetry energy at saturation for any value of the NS mass, very weak correlations seem to exist with the derivative of the nuclear symmetry energy and with the nuclear incompressibility.

scholarly journals Symmetry Energy and the Pauli Exclusion Principle

Symmetry ◽  
2021 ◽  
Vol 13 (11) ◽  
pp. 2116
Author(s):  
Claudio O. Dorso ◽  
Guillermo Frank ◽  
Jorge A. López
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Pauli Exclusion Principle ◽  
Nucleon Nucleon ◽  
Binding Energies ◽  
Exclusion Principle ◽  
Neutron Star Matter ◽  
Intermediate Energies ◽  
Metropolis Monte Carlo ◽  
Finite Nuclei

In this article we present a classical potential that respects the Pauli exclusion principle and can be used to describe nucleon-nucleon interactions at intermediate energies. The potential depends on the relative momentum of the colliding nucleons and reduces interactions at low momentum transfer mimicking the Pauli exclusion principle. We use the potential with Metropolis Monte Carlo methods and study the formation of finite nuclei and infinite systems. We find good agreement in terms of the binding energies, radii, and internal nucleon distribution of finite nuclei, and the binding energy in nuclear matter and neutron star matter, as well as the formation of nuclear pastas, and the symmetry energy of neutron star matter.

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.

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