Isospin-dependent properties of asymmetric nuclear matter in relativistic mean field models

Effects of the ω meson self coupling (OMSC) on the thermal properties of asymmetric nuclear matter (ANM) are studied within the framework of relativistic mean field (RMF) model that includes contributions of all possible mixed interactions among meson fields involved up to quartic order. In particular, we study the mechanical and chemical instabilities (spinodal), as well as the liquid-gas phase transition (binodal) at finite temperature. It is found that the onset of spinodal instabilities and the binodal curve are only marginally affected by variation of the OMSC parameter, whereas the binodal curve shows a strong correlation to the symmetry energy. Comparison with other ERMF parameter sets is also performed.

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Hyperons in a relativistic mean-field approach to asymmetric nuclear matter

Physical Review C ◽

10.1103/physrevc.70.054309 ◽

2004 ◽

Vol 70 (5) ◽

Cited By ~ 32

Author(s):

J. Kotulič Bunta ◽

Štefan Gmuca

Keyword(s):

Nuclear Matter ◽

Mean Field ◽

Asymmetric Nuclear Matter ◽

Field Approach ◽

Relativistic Mean Field

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δ MESON EFFECTS ON ASYMMETRIC NUCLEAR MATTER

International Journal of Modern Physics E ◽

10.1142/s0218301308010805 ◽

2008 ◽

Vol 17 (09) ◽

pp. 1815-1824 ◽

Cited By ~ 4

Author(s):

B. LIU ◽

M. DI TORO ◽

V. GRECO

Keyword(s):

Neutron Stars ◽

Nuclear Matter ◽

Mean Field ◽

Coupling Scheme ◽

Asymmetric Nuclear Matter ◽

Density Dependent ◽

Remarkable Effect ◽

Relativistic Mean Field ◽

The Stability ◽

The Impact

The impact of a δ meson field (the scalar-isovector channel) on asymmetric nuclear matter is studied within relativistic mean-field (RMF) models with both constant and density dependent (DD) nucleon-meson couplings. The Equation of State (EOS) for asymmetric nuclear matter and the neutron star properties by the different models are compared. We find that the δ-field in the constant coupling scheme leads to a larger repulsion in dense neutron-rich matter and to a definite splitting of proton and neutron effective masses, finally influencing the stability of the neutron stars. A broader analysis of possible δ-field effects is achieved considering also density dependent nucleon-meson coupling. A remarkable effect on the relation between mass and radius for the neutron stars is seen, showing a significant reduction of the radius along with a moderate mass reduction due to the increase of the effective δ coupling in high density regions.

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Skyrme and Relativistic Mean-Field Models in the Description of Symmetric, Asymmetric, and Stellar Nuclear Matter

Nuclear Structure Physics ◽

10.1201/9780429288647-2 ◽

2020 ◽

pp. 27-65

Author(s):

O. Lourenço ◽

M. Dutra ◽

P. D. Stevenson

Keyword(s):

Nuclear Matter ◽

Mean Field ◽

Relativistic Mean Field ◽

Mean Field Models

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Beta Equilibrium Under Neutron Star Merger Conditions

Universe ◽

10.3390/universe7110399 ◽

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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