Equation of state of isospin-asymmetric nuclear matter in relativistic mean-field models with chiral limits

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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NEUTRON STAR MASS CORRELATION WITH SOUND VELOCITY AND INCOMPRESSIBILITY AT THE STAR CENTER IN THE POLYTROPIC APPROXIMATION

International Journal of Modern Physics D ◽

10.1142/s0218271810017974 ◽

2010 ◽

Vol 19 (08n10) ◽

pp. 1575-1582

Author(s):

L. FERRARI ◽

P. C. R. ROSSI ◽

M. MALHEIRO

Keyword(s):

Neutron Star ◽

Equation Of State ◽

Nuclear Matter ◽

Sound Velocity ◽

Mean Field ◽

Star Mass ◽

Mean Field Models ◽

Neutron Star Mass ◽

Analytic Expressions ◽

Walecka Model

In this paper we use a polytropic approximation to the equation of state for the interior of neutrons stars, described by relativistic hadronic mean field models. In this approximation, it is possible to obtain analytic expressions for the sound velocity and the incompressibility at the star center. We found a correlation between these quantities and the star mass. Using two well-known parametrizations of the nonlinear Walecka model for nuclear matter composed only of protons, neutrons and electron in β equilibrium, we obtain for a star mass of 1.43 M⊙ a central incompressibility Kc = (3000±100), around ten times the nuclear matter incompressibility, and a central sound velocity (v/c)2 ~ 0.3.

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Vlasov formalism for extended relativistic mean field models: The crust-core transition and the stellar matter equation of state

Physical Review C ◽

10.1103/physrevc.94.015808 ◽

2016 ◽

Vol 94 (1) ◽

Cited By ~ 24

Author(s):

Helena Pais ◽

Constança Providência

Keyword(s):

Equation Of State ◽

Mean Field ◽

Stellar Matter ◽

Relativistic Mean Field ◽

Mean Field Models

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THE NUCLEON STRUCTURE AND THE EQUATION OF STATE FOR NUCLEAR MATTER

International Journal of Modern Physics E ◽

10.1142/s0218301307006058 ◽

2007 ◽

Vol 16 (02) ◽

pp. 608-615

Author(s):

J. ROŻYNEK

Keyword(s):

Equation Of State ◽

Structure Function ◽

Nuclear Matter ◽

Mean Field ◽

Nucleon Structure ◽

Final State ◽

Rest Energy ◽

Relativistic Mean Field ◽

Quark Contribution ◽

Nucleon Structure Function

We show the density dependent corrections to the nucleon structure function in the frame of nuclear Relativistic Mean Field (RMF) models. These corrections are connected with the modifications of the parton distribution in nuclei emerging from generalized nuclear Fermi motion and final state interactions between the nucleon and the rest of the nucleus. The medium effects concern the nucleon structure, namely the changes in the nucleon rest energy, the enhancement of sea quark contribution (simulated with "nuclear pions") and the modifications of the transverse parton momentum distribution inside Nuclear Matter (NM). The sea parton distributions are described by the modified cloud of virtual pions in order to saturate the nuclear energy-momentum sum rule. The description of theses features are in good agreement with experimental data; the EMC effect for x > 0.15 and nuclear lepton pair production data has been described essentialy without free parameters. The influence of these medium modifications to the nucleon structure function within the equation of state in RMF models of NM will be discussed.

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