Hot nuclear and neutron matter with a density-dependent interaction

Das, Chinmay; Tripathi, R. K.; Sahu, R.

doi:10.1103/physrevc.45.2217

Cited by 22 publications

(35 citation statements)

References 13 publications

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“…However, when they include the Urbana three-nucleon potential in the calculations they find, in contrast with our result, that three-body forces do not strongly affect the critical temperature, which is reduced to T c ≃ 20 MeV. Other calculations within the Bloch-de Dominicis formalism [28] or the relativistic Dirac-Brückner-Hartree-Fock approach [5,29], on the other hand, yield lower values of T c , respectively 9, 12 and 10.4 MeV, closer to our result with three-body forces.…”

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confidence: 99%

Thermodynamic properties of nuclear matter with three-body forces

Somà

Božek

2009

Phys. Rev. C

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We calculate thermodynamic quantities in symmetric nuclear matter within the self-consistent Green's functions method including three-body forces. The thermodynamic potential is computed directly from a diagrammatic expansion, implemented with the CD-Bonn and Nijmegen nucleonnucleon potentials and the Urbana three-body forces. We present results for entropy and pressure up to temperatures of 20 MeV and densities of 0.32 fm −3 . While the pressure is sensitive to the inclusion of three-body forces, the entropy is not. The unstable spinodal region is identified and the critical temperature associated to the liquid-gas phase transition is determined. When three-body forces are added we find a strong reduction of the critical temperature, obtaining Tc ≃ 12 MeV. The determination of thermodynamic properties of hot nuclear matter is extremely relevant for its applications in astrophysics and heavy-ion reactions. Pressure and entropy at finite temperature are crucial ingredients in the modeling of core-collapse supernovae and protoneutron stars, which involve processes characterized by densities up to several time the nuclear saturation density and temperatures up to few tens of MeV's. The nuclear equation of state (EOS) plays an important role also in the interpretation of nucleus-nucleus collisions, in which a hot and dense state of matter is formed. Of particular interest is the study of a possible phase transition occurring at subsaturation densities. Because of the van der Waals nature of nucleon-nucleon (NN) interactions, at low densities and high temperatures nuclear matter is expected to undergo a first-order transition to a gas phase [1]. It is claimed that an evidence for such behavior is found in intermediate energy heavy ion collisions, as a plateau of the caloric curve derived for the light fragments as a function of the reaction energy [2].The liquid-gas transition in nuclear matter presents some differences with respect to the case of finite nuclei where, as the temperature increases, Coulomb forces together with the decrease of the surface tension trigger the onset of mechanical instabilities. One can try to relate the limiting temperature of nuclei T l to the critical temperature in infinite matter T c by properly taking into account Coulomb and surface effects [3]. Different estimates from effective models based on Skyrme forces [4] and more microscopic approaches [5,6] are in agreement and yield a ratio T l /T c of about 1/3.A reliable many-body theory is called for the interpretation of the heavy ion reactions in the goal of extracting the equation of state and the critical point of the nuclear liquid-gas phase transition [7] and in order to extrapolate to higher densities and arbitrary isospin asymme- * Electronic address : vittorio.soma@ifj.edu.pl † Electronic address : piotr.bozek@ifj.edu.pl tries. There exist only few realistic calculations of the nuclear matter EOS at finite temperature. The variational approach, which yields reliable results at T = 0, is usually extended to finite temperatures...

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confidence: 99%

Thermodynamic properties of nuclear matter with three-body forces

Somà

Božek

2009

Phys. Rev. C

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“…The relativistic mean-field theory have been applied by Prakash and Ainsworth [12], Serot and Walecka [13], Muller and Serot [14], Freedman [15] and Wang [16]. The variational theory of quantum fluids have been used by Friedman and Pandharipande [17], Wringa et al [18], and the Brueckner theory calculation with various phenomenological interactions have been carried out by Baldo et al [19,45], Das et al [20] and Bombaci et al [21], Bombaci and Lombardo [22] and Zuo et al [23]. The chiral Sigma model have been applied by Jena and Singh [24], and Sahu et al [25], and the relativistic BrucknerHartree-Fock theory at finite temperature have been applied by Weber et al [9].…”

Section: Introductionmentioning

confidence: 99%

Thermal properties of asymmetrical nuclear matter with the new charge-dependent Reid potential

Moshfegh

Modarres

2007

Nuclear Physics A

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“…The absence of neutrino-trapping has a dramatic effect on the equation of state and is the main cause of a significant reduction in the values of the proton fraction Y p [27,36]. The chemical equilibrium of reactions (24) can be expressed in terms of the chemical potentials for the four species…”

Section: β-Equilibrium In Hot Proto-neutron Star and Supernovamentioning

confidence: 99%

“…There is a wealth of existing literature regarding the EOS of supernova matter [1,4,7,8,9,10,11,12,13,14,15,16,17,18,19,20,21,22,23,24,25,26,27,28,29,30,31]. Supernova matter which exists in a collapsing supernova core and eventually forms a hot neutron star at birth is another form of nuclear matter distinguished in the participation of degenerate neutrinos and electrons [27].…”

Section: Introductionmentioning

confidence: 99%

Equation of State for Dense Supernova Matter

Moustakidis

2009

Int. J. Mod. Phys. D

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We provide an equation of state for high density supernova matter by applying a momentumdependent effective interaction. We focus on the study of the equation of state of high-density and high-temperature nuclear matter containing leptons (electrons and neutrinos) under the chemical equilibrium condition. The conditions of charge neutrality and equilibrium under β-decay process lead first to the evaluation of the lepton fractions and afterwards the evaluation of internal energy, pressure, entropy and in total to the equation of state of hot nuclear matter for various isothermal cases. Thermal effects on the properties and equation of state of nuclear matter are evaluated and analyzed in the framework of the proposed effective interaction model. Since supernova matter is characterized by a constant entropy we also present the thermodynamic properties for isentropic case. Special attention is dedicated to the study of the contribution of the components of β-stable nuclear matter to the entropy per particle, a quantity of great interest for the study of structure and collapse of supernova. PACS number(s): 21.65.+f, 21.30.Fe, 24.10.Pa, 26.60.+c, 26.50.+x, 26.60.Kp

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Hot nuclear and neutron matter with a density-dependent interaction

Cited by 22 publications

References 13 publications

Thermodynamic properties of nuclear matter with three-body forces

Thermodynamic properties of nuclear matter with three-body forces

Thermal properties of asymmetrical nuclear matter with the new charge-dependent Reid potential

Equation of State for Dense Supernova Matter

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