Isospin-dependent clusterization of neutron-star matter

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

doi:10.1016/j.nuclphysa.2007.03.006

Cited by 85 publications

(117 citation statements)

References 33 publications

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“…For a more detailed discussion on the symmetry energy and temperature effects on the spinodal region, we refer readers to Refs. [30][31][32][33][34][35]. The following analysis of the transition density and pressure in hot neutron stars is, however, carried out by using the more realistic dynamical approach.…”

Section: Locating the Inner Edge Of The Neutron Star Crustmentioning

confidence: 99%

Transition density and pressure in hot neutron stars

et al. 2010

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Using the momentum-dependent effective interaction (MDI) for nucleons, we have studied the transition density and pressure at the boundary between the inner crust and the liquid core of hot neutron stars. We find that their values are larger in neutrino-trapped neutron stars than in neutrino-free neutron stars. Furthermore, both are found to decrease with increasing temperature of a neutron star as well as increasing slope parameter of the nuclear symmetry energy, except that the transition pressure in neutrino-trapped neutron stars for the case of small symmetry energy slope parameter first increases and then decreases with increasing temperature. We have also studied the effect of the nuclear symmetry energy on the critical temperature above which the inner crust in a hot neutron star disappears and found that with increasing value of the symmetry energy slope parameter, the critical temperature decreases slightly in neutrino-trapped neutron stars but first decreases and then increases in neutrino-free neutron stars.

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Section: Locating the Inner Edge Of The Neutron Star Crustmentioning

confidence: 99%

Transition density and pressure in hot neutron stars

et al. 2010

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“…For this reason the convexity analysis of the thermodynamical potential in the extensive variable space has been often employed to spot the presence of phase transitions, e.g. for the neutron-proton system [42,43]. At zero temperature, one thermodynamic potential is given by the total energy…”

Section: Phase Diagram Of the Two-component N − λ Systemmentioning

confidence: 99%

Phase transition toward strange matter

2012

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The phase diagram of a system constituted of neutrons and Λ-hyperons in thermal equilibrium is evaluated in the mean-field approximation. It is shown that this simple system exhibits a complex phase diagram with first and second order phase transitions. Due to the generic presence of attractive and repulsive couplings, the existence of phase transitions involving strangeness appears independent of the specific interaction model. In addition we will show under which conditions a phase transition towards strange matter at high density exists, which is expected to persist even within a complete treatment including all the different strange and non-strange baryon states. The impact of this transition on the composition of matter in the inner core of neutron stars is discussed.

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“…3, isospin distillation is particularly affected at low values of q, where Coulomb effects dominate: an inverse distillation is even found near the low-q border of the instability interval. However, the normal isospin distillation remains the dominant feature, especially if we consider the most unstable modes [21,44]: it leads to the formation of clusters more symmetric than the homogeneous initial system, immersed in a more neutron-rich gas. Figure 3 shows a very close agreement between Vlasov and RPA results as for the value of δρ 3 /δρ.…”

Section: A Unstable Eigen-modesmentioning

confidence: 99%

“…The spinodal decomposition studied in this framework can be related to the nuclear multifragmentation process by neglecting the finite size of the homogeneous medium formed in the early stage of the collision. It also gives a picture of the instability against clusterization in compact-star matter, where the degree of freedom associated with the electrons can be neglected [21].…”

Section: Introductionmentioning

confidence: 99%

“…Starting from the thermodynamic definition of the liquid-gas phase transition, we first concentrate on the free-energy curvature properties. This leads us to study the finite-size density fluctuations in a Thomas-Fermi approach [21,22], defining a static criterion for the existence of instabilities based on the free-energy variations. Afterward, consistently with this local equilibrium framework, we treat the time evolution by introducing hydrodynamical equations.…”

Section: Introductionmentioning

confidence: 99%

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Cluster formation in asymmetric nuclear matter: Semi-classical and quantal approaches

2008

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The nuclear-matter liquid-gas phase transition induces instabilities against finite-size density fluctuations. This has implications for both heavy-ion-collision and compact-star physics. In this paper, we study the clusterization properties of nuclear matter in a scenario of spinodal decomposition, comparing three different approaches: the quantal RPA, its semi-classical limit (Vlasov method), and a hydrodynamical framework. The predictions related to clusterization are qualitatively in good agreement varying the approach and the nuclear interaction. Nevertheless, it is shown that i) the quantum effects reduce the instability zone, and disfavor short-wavelength fluctuations; ii) large differences appear between the two semi-classical approaches, which correspond respectively to a collisionless (Vlasov) and local equilibrium description (hydrodynamics); iii) the isospin-distillation effect is stronger in the local equilibrium framework; iv) important variations between the predicted time-scales of cluster formation appear near the borders of the instability region.

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Isospin-dependent clusterization of neutron-star matter

Cited by 85 publications

References 33 publications

Transition density and pressure in hot neutron stars

Transition density and pressure in hot neutron stars

Phase transition toward strange matter

Cluster formation in asymmetric nuclear matter: Semi-classical and quantal approaches

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