Critical properties of symmetric nuclear matter in low-density regime using effective-relativistic mean field formalism

Abstract

The effective field theory motivated relativistic mean-field (E-RMF) formalism is employed to study the equation of state (EoS) for the infinite symmetric nuclear matter (SNM) at finite temperature using the recently developed forces FSUGarnet, IOPB-I, G3, and the well known NL3 force parameter. The EoS is then used to estimate the critical temperature T c, pressure P c and density ρ c of the SNM for the liquid–gas phase transition. As T c is not a constrained parameter in both experiments and theoretical calculations, there is a large uncertainty around its value. Although, the critical parameters are correlated among themselves. It is revealed that vector self-coupling ζ 0 of used forces play determining role in EoS in finite temperature limit. Keeping the incompressibility in acceptable limit i.e. 240 ± 20 MeV, the lower value of ζ 0 gives a better result of T c when compared to the several experimental data. The critical parameters however show weak correlation with the properties at saturation density at zero temperature. The compressibility factors calculated with these parameters are in agreement with the universal value of liquid–gas systems. Stability conditions are examined along with binodal and spinodal regions. Besides this, the thermodynamic properties like specific heat and latent heat are also worked out. We have carried out detailed consistency check of our calculations using critical exponents and standard scaling laws. All the exponents are well within the theoretical mean-field results.

Crustal properties of a neutron star within an effective relativistic mean-field model

“…This formalism has been applied in a wide range of nuclear physics problems in the past few years [59][60][61][62][63][64]. The E-RMF effective Lagrangian which include the interaction between different mesons, such as, σ, ω, ρ, δ and photon is written as [47,50,[65][66][67][68],…”

Crustal properties of a neutron star within an effective relativistic mean-field model

“…Thus discontinuity in density suggests the transition from one layer of the nucleus to another. One also gets rid of the Maxwell construction [60] to determine the transition pressure from one nucleus to another. The pressure can be calculated from the first law of thermodynamics as [49]…”

“…In this case, the interaction between different mesons, such as, σ, ω, ρ and δ is included up to fourth order. The photon field is also included with E-RMF energy density functional as [29,54,60,[64][65][66]…”

Properties of hot finite nuclei and associated correlations with infinite nuclear matter

“…6 MeV for the mass region A ≈ 90 in ALADIN experiment [11]. Nuclear multi-fragmentation occurs in the region of spinodal or phase instability boundary in the nuclear matter phase diagram [12]. The nucleus, which resembles a hot liquid drop, expands because of thermal pressure and moves to the spinodal region where it is surrounded by a nucleon gas.…”

“…The temperature-dependent surface energy term depends on the T c which is calculated for these individual E-RMF parameter sets. In the analysis of critical properties of infinite nuclear matter using these E-RMF sets in [12], we found that the T c is not a well-constrained quantity and the majority of E-RMF sets that satisfy the relevant observational and experimental constraints on EoS underestimates it. Since the experimental value of T c is calculated by extrapolating the data from multifragmentation reaction data on finite nuclei, it is interesting to see the variation of T l of finite nuclei using different E-RMF forces.…”