On the density-dependent hadron field theory at finite temperature and its thermodynamical consistency

Avancini, S. S.; Bracco, Mirian E.; Chiapparini, M.; Menezes, D. P.

doi:10.1088/0954-3899/30/2/003

Cited by 9 publications

(10 citation statements)

References 20 publications

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“…The prototype of such theory is Quantum Hadrodynamics (QHD) [20,21], which has been shown to describe well many properties of nuclear matter, finite nuclei and neutron stars [20,21,23,24,25,26,27]. This theory can be extended to include many-body correlations as density-dependent meson couplings [28,29]. The successful description of nuclear properties indicates that the essential aspects of low energy strong interactions are well described by QHD.…”

Section: Introductionmentioning

confidence: 99%

Hadron production in non-linear relativistic mean field models

et al. 2009

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By using a parametrization of the non-linear Walecka model which takes into account the binding energy of different hyperons, we present a study of particle production yields measured in central Au-Au collision at RHIC. Two sets of different hyperon-meson coupling constants are employed in obtaining the hadron production and chemical freeze-out parameters. These quantities show a weak dependence on the used hyperon-meson couplings. Results are in good overall accordance with experimental data. We have found that the repulsion among the baryons is quite small and, through a preliminary analysis of the effective mesonic masses, we suggest a way to improve the fittings.

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Section: Introductionmentioning

confidence: 99%

Hadron production in non-linear relativistic mean field models

et al. 2009

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“…The important range of temperature which is discussed lies between 10 and 150 MeV since the liquid-gas phase transition takes place around 10 MeV, the phase transition from hadronic to quarkionic matter around 150 MeV and the relevant temperatures in the cooling of a protoneutron star after a supernova explosion takes place go up to approximately 40 MeV [16]. In this work we discuss another possible application of the formalism we have derived in [14,15] in order to incorporate temperature effects in the study of lagrangians with BR scaling.…”

Section: Introductionmentioning

confidence: 99%

“…We have already shown that one of these density dependent models, to which we refer as TW model [12,13], originally derived at T = 0 can be extrapolated to finite temperatures once the thermodynamical consistency remains unaltered [14,15]. The important range of temperature which is discussed lies between 10 and 150 MeV since the liquid-gas phase transition takes place around 10 MeV, the phase transition from hadronic to quarkionic matter around 150 MeV and the relevant temperatures in the cooling of a protoneutron star after a supernova explosion takes place go up to approximately 40 MeV [16].…”

Section: Introductionmentioning

confidence: 99%

Density dependent parametrization models: Formalism and applications

Avancini

Menezes

2006

Phys. Rev. C

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In this work we derive a formalism to incorporate asymmetry and temperature effects in the Brown-Rho (BR) scaled lagrangian model in a mean field theory. The lagrangian density discussed in this work requires less parameters than the usual models with density dependent couplings. We also present the formalism with the inclusion of the eight lightest baryons, two lightest leptons, β equilibrium and charge neutrality in order to apply the BR scaled model to the study of neutron stars. The results are again compared with the ones obtained from another density dependent parametrization model. The role played by the rearrangement term at T=0 for nuclear or neutron star matter and at finite temperature is investigated. The BR scaled model is shown to be a good tool in studies involving density dependent effective masses and in astrophysics applications.PACS number(s): 21.65.+f, 24.10.Jv,26.60.+c,21.30.Fe

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“…This term guarantees the thermodynamical consistency and the energy-momentum conservation. For more detailed calculations, at zero and finite temperatures, please refer to [41].…”

Section: The Tw Density Dependent Hadronic Modelmentioning

confidence: 99%

Density dependent hadronic models and the relation between neutron stars and neutron skin thickness

et al. 2007

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In the present work, we investigate the main differences in the lead neutron skin thickness, binding energy, surface energy, and density profiles obtained with two different density dependent hadron models. Our results are calculated within the Thomas-Fermi approximation with two different numerical prescriptions and compared with results obtained with a common parametrization of the nonlinear Walecka model. The neutron skin thickness is a reflex of the equation of state properties. Hence, a direct correlation is found between the neutron skin thickness and the slope of the symmetry energy. We show that within the present approximations, the asymmetry parameter for low momentum transfer polarized electron scattering is not sensitive to the model differences. DOI: 10.1103/PhysRevC.75.055805 PACS number(s): 21.65.+f, 24.10.Jv, 95.30.Tg, 26.60.+c 055805-2 DENSITY DEPENDENT HADRONIC MODELS AND THE . . . PHYSICAL REVIEW C 75, 055805 (2007)

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On the density-dependent hadron field theory at finite temperature and its thermodynamical consistency

Cited by 9 publications

References 20 publications

Hadron production in non-linear relativistic mean field models

Hadron production in non-linear relativistic mean field models

Density dependent parametrization models: Formalism and applications

Density dependent hadronic models and the relation between neutron stars and neutron skin thickness

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