Role of isospin in the nuclear liquid–gas phase transition

Ducoin, C.; Chomaz, Ph.; Gulminelli, F.

doi:10.1016/j.nuclphysa.2006.03.005

Cited by 78 publications

(125 citation statements)

References 25 publications

(14 reference statements)

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“…Matter stability with respect to phase separation can be checked in any point of the extensive variable space by analyzing the eigen-values of the curvature matrix [5,30,31], C ij = ∂ 2 f ({n l } l={i,j,k} )/∂n i ∂n j , where i, j, k = B, S, Q and f = e tot − T s tot is the total freeenergy. The occurrence of, at least, one negative eigenvalue in a certain domain of (n B , n S , n Q ) means that the system is unstable versus phase separation.…”

Section: B Instabilities and Phase-transitionmentioning

confidence: 99%

“…The occurrence of, at least, one negative eigenvalue in a certain domain of (n B , n S , n Q ) means that the system is unstable versus phase separation. The associated 3-dimensional Gibbs construction can be reduced to a simpler 1-dimensional Maxwell construction [5] by performing a Legendre transformation with respect to two out of the three chemical potentials µ B = µ n , µ S = −µ Λ + µ n and µ Q = µ p − µ n . We have chosen to work in the hybrid ensemble (n B , µ S , µ Q ) defined by:…”

Section: B Instabilities and Phase-transitionmentioning

confidence: 99%

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Strangeness-driven phase transition in (proto-)neutron star matter

et al. 2013

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The phase diagram of a system constituted of neutrons, protons, Λ-hyperons and electrons is evaluated in the mean-field approximation in the complete three-dimensional space given by the baryon, lepton and strange charge. It is shown that the phase diagram at sub-saturation densities is strongly affected by the electromagnetic interaction, while it is almost independent of the electric charge at supra-saturation density. As a consequence, stellar matter under the condition of strangeness equilibrium is expected to experience a first as well as a second-order strangeness-driven phase transition at high density, while the liquid-gas phase transition is expected to be quenched. An RPA calculation indicates that the presence of this critical point might have sizable implications for the neutrino propagation in core-collapse supernovae.

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Section: B Instabilities and Phase-transitionmentioning

confidence: 99%

Section: B Instabilities and Phase-transitionmentioning

confidence: 99%

Strangeness-driven phase transition in (proto-)neutron star matter

et al. 2013

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“…If this is the case, the spinodal zone is not directly pertinent for star-matter thermodynamics. However the spinodal region contains points of locally inversed curvature, and is always by construction included inside the region of globally inversed curvature, namely the coexistence zone [9,11].…”

Section: Global Instability Of Homogeneous Mattermentioning

confidence: 99%

“…where the coefficients C i an D i are linear combinations of the standard Skyrme parameters [11,21]. The mean field is given by the expression :…”

Section: Global Instability Of Homogeneous Mattermentioning

confidence: 99%

“…In laboratory experiments, this phase diagram can be explored only through heavy-ion collisions; in particular the multifragmentation phenomenon, observed for collisions around the Fermi energy and above, has been interpreted as the occurrence of the nuclear liquid-gas phase transition rounded by finite-size effects [4,5,6,7,8]. From the theoretical point of view, the isospin properties of the phase diagram have been studied extensively [9,10,11] and we know that the phase transition concerns isospin-symmetric (ρ n = ρ p ) as well as asymmetric (ρ n = ρ p ) matter.…”

Section: Introductionmentioning

confidence: 99%

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Isospin-dependent clusterization of neutron-star matter

2007

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Because of the presence of a liquid-gas phase transition in nuclear matter, compactstar matter can present a region of instability against the formation of clusters. We investigate this phase separation in a matter composed of neutrons, protons and electrons, within a Skyrme-Lyon mean-field approach. Matter instability and phase properties are characterized through the study of the free-energy curvature. The effect of β-equilibrium is also analyzed in detail, and we show that the opacity to neutrinos has an influence on the presence of clusterized matter in finite-temperature proto-neutron stars.

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Isospin fractionation: Equilibrium versus spinodal decomposition

2007

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This paper focuses on the isospin properties of the asymmetric nuclear-matter liquid-gas phase transition analyzed in a mean-field approach, using Skyrme effective interactions. We compare two different mechanisms of phase separation for low-density matter: equilibrium and spinodal decomposition. The isospin properties of the phases are deduced from the free-energy curvature, which contains information both on the average isospin content and on the system fluctuations. Some implications on experimentally accessible isospin observables are presented.

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Role of isospin in the nuclear liquid–gas phase transition

Cited by 78 publications

References 25 publications

Strangeness-driven phase transition in (proto-)neutron star matter

Strangeness-driven phase transition in (proto-)neutron star matter

Isospin-dependent clusterization of neutron-star matter

Isospin fractionation: Equilibrium versus spinodal decomposition

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