scholarly journals A microscopic estimate of the nuclear matter compressibility and symmetry energy in relativistic mean-field models

2003 ◽  
Vol 68 (2) ◽  
Author(s):  
D. Vretenar ◽  
T. Nikšić ◽  
P. Ring
Keyword(s):  
Nuclear Matter ◽  
Symmetry Energy ◽  
Mean Field ◽  
Relativistic Mean Field ◽  
Mean Field Models

scholarly journals Relativistic mean-field models and nuclear matter constraints

2013 ◽  
Author(s):  
M. Dutra ◽  
O. Lourenço ◽  
B. V. Carlson ◽  
A. Delfino ◽  
D. P. Menezes ◽  
...  
Keyword(s):  
Nuclear Matter ◽  
Mean Field ◽  
Relativistic Mean Field ◽  
Mean Field Models

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 Consistent relativistic mean-field models: symmetry energy parameter

2019 ◽  
Vol 1291 ◽  
pp. 012043
Author(s):  
O Lourenço ◽  
M Dutra ◽  
O Hen ◽  
E Piasetzky ◽  
D P Menezes
Keyword(s):  
Symmetry Energy ◽  
Mean Field ◽  
Energy Parameter ◽  
Relativistic Mean Field ◽  
Mean Field Models

CONSTRAINING THE DENSITY DEPENDENCE OF THE SYMMETRY ENERGY WITH NUCLEAR STRUCTURE PROPERTIES

2010 ◽  
Vol 19 (08n09) ◽  
pp. 1720-1726
Author(s):  
WEI-ZHOU JIANG
Keyword(s):  
Nuclear Matter ◽  
Density Dependence ◽  
Symmetry Energy ◽  
Field Model ◽  
Mean Field ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Finite Nuclei ◽  
The Relationship ◽  
Structure Properties

In this work, we review a few structural properties in finite nuclei and nuclear matter that are sensitive to differences in the symmetry energy, and discuss mechanisms that can enhance the sensitivity to differences in the symmetry energy with the relativistic mean-field model. Emphasis has been placed on the establishment of the relationship between the deexcitation energy of superdeformed secondary minima and the density dependence of the symmetry energy.

scholarly journals Beta Equilibrium Under Neutron Star Merger Conditions

Universe ◽  
2021 ◽  
Vol 7 (11) ◽  
pp. 399
Author(s):  
Mark G. Alford ◽  
Alexander Haber ◽  
Steven P. Harris ◽  
Ziyuan Zhang
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Equilibrium Condition ◽  
Mean Field ◽  
Temperature Correction ◽  
Nonzero Temperature ◽  
Relativistic Mean Field ◽  
Mean Field Models ◽  
Relativistic Dispersion ◽  
Correct Calculation

We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1MeV<T≲5MeV. We improve on previous work using a consistent description of nuclear matter based on the IUF and SFHo relativistic mean field models. This includes using relativistic dispersion relations for the nucleons, which we show is essential in these models. We find that the nonzero-temperature correction can be of order 10 to 20 MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of 10 or more if it is neglected.

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