Structure of Matter below Nuclear Saturation Density

Ravenhall, D. G.; Pethick, C. J.; Wilson, J. R.

doi:10.1103/physrevlett.50.2066

Cited by 666 publications

(826 citation statements)

References 6 publications

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“…Spherical nuclei turn out to be energetically preferred over other nuclear shapes, and also over homogeneous npe matter, down to ρ crit = 0.077 fm −3 . Therefore, within our set of possible nuclear shapes, the ground state of neutron-star crust contains spherical nuclei, down to its bottom edge.As was already noticed in [28,29,17], exotic nuclei will be present only if the filling fraction, u, is large enough. For a given neutron excess, introducing finite size (Coulomb and surface) effects increases the value of u.…”

mentioning

confidence: 84%

Inner edge of neutron-star crust with SLy effective nucleon-nucleon interactions

2000

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mentioning

confidence: 84%

Inner edge of neutron-star crust with SLy effective nucleon-nucleon interactions

2000

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“…Clustering is also expected to play an important role in compact stars [9,10]. It is predicted to lead to the presence of complex structures like the "pasta phases" occurring in the inner crust of neutron stars [11,12,13,14]. At lower densities and finite temperature, star matter may clusterize into light nuclei [15,16].…”

Section: Introductionmentioning

confidence: 99%

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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“…In particular neutron-star properties may be influenced by the presence of exotic "pasta phases" in their inner crust [14,15,16,17].…”

Section: Introductionmentioning

confidence: 99%

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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Structure of Matter below Nuclear Saturation Density

Cited by 666 publications

References 6 publications

Inner edge of neutron-star crust with SLy effective nucleon-nucleon interactions

Inner edge of neutron-star crust with SLy effective nucleon-nucleon interactions

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

Isospin-dependent clusterization of neutron-star matter

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