Low-density instabilities in relativistic asymmetric matter of compact stars

Providência, Constança; Brito, L.; Avancini, S. S.; Menezes, D. P.; Chomaz, Ph.

doi:10.1103/physrevc.73.025805

Cited by 67 publications

(94 citation statements)

References 44 publications

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“…It is shown that pasta clusters in β equilibrium completely melt for temperatures above 5 to 6 MeV. These results agree partially with the predictions obtained within a dynamical spinodal (DS) approach [24][25][26]. A similar calculation was done with Skyrme forces in Ref.…”

Section: Introductionsupporting

confidence: 80%

“…In the latter case, the crust-core transition is defined by the intersection between the β-equilibrium EoS and the dynamical spinodal (DS). The cluster size is identified with half the wavelength of the density fluctuation [24,25,27]. The results are shown in Fig.…”

Section: Finite-temperature Effects On Crustmentioning

confidence: 93%

“…We perform the study by using both a finite-temperature TF calculation of the pasta phase and the finite-temperature dynamical approach within the relativistic Vlasov formalism [24][25][26]47]. In the latter case, the crust-core transition is defined by the intersection between the β-equilibrium EoS and the dynamical spinodal (DS).…”

Section: Finite-temperature Effects On Crustmentioning

confidence: 99%

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Equation of state and thickness of the inner crust of neutron stars

et al. 2014

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The cell structure of β-stable clusters in the inner crust of cold and warm neutron stars is studied within the Thomas-Fermi approach by using relativistic mean-field nuclear models. The relative size of the inner crust and the pasta phase of neutron stars is calculated, and the effect of the symmetry energy slope parameter L on the profile of the neutron star crust is discussed. It is shown that, while the size of the total crust is mainly determined by the incompressibility modulus, the relative size of the inner crust depends on L. It is found that the inner crust represents a larger fraction of the total crust for smaller values of L. Finally, it is shown that, at finite temperature the pasta phase in β-equilibrium matter essentially melts above 5 to 6 MeV, and that the onset density of the rod-like and slab-like structures does not depend on the temperature.

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Section: Introductionsupporting

confidence: 80%

Section: Finite-temperature Effects On Crustmentioning

confidence: 93%

Section: Finite-temperature Effects On Crustmentioning

confidence: 99%

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Equation of state and thickness of the inner crust of neutron stars

et al. 2014

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“…[17] and references therein. Matter is stable to fluctuations in density and composition, under conditions of constant volume and temperature, when the free energy density F is a convex function of the proton and neutron densities.…”

Section: B Thermodynamical Instabilitiesmentioning

confidence: 99%

“…The nuclear pasta phases can be thought of as arising due to unstable collective modes in uniform matter [14], with the transition to uniform matter studies by analyzing the dynamical and thermodynamical spinodals in density and temperature space [15][16][17][18]. To study the details of the pasta phases themselves, modeling of the inhomogeneous phases is required.…”

Section: Introductionmentioning

confidence: 99%

Phase transitions in core-collapse supernova matter at sub-saturation densities

2014

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Phase transitions in hot, dense matter in the collapsing core of massive stars have an important impact on the core-collapse supernova mechanism as they absorb heat, disrupt homology and so weaken the developing shock. We perform a three-dimensional, finite temperature SkyrmeHartree-Fock (SHF) study of inhomogeneous nuclear matter to determine the critical density and temperature for the phase transition between the pasta phase and homogeneous matter and its properties. We employ four different parametrizations of the Skyrme nuclear energy-density functional, SkM * , SLy4, NRAPR and SQMC700, which span a range of saturation-density symmetry energy behaviours constrained by a variety of nuclear experimental probes. For each of these interactions we calculate free energy, pressure, entropy and chemical potentials in the range of particle number densities where the nuclear pasta phases are expected to exist, 0.02 -0.12 fm −3 , temperatures 2 -8 MeV and a proton fraction of 0.3. We find unambiguous evidence for a first-order phase transition to uniform matter, unsoftened by the presence of the pasta phases. No conclusive signs of first-order phase transition between the pasta phases is observed, and it is argued that the thermodynamic quantities vary continuously right up to the first-order phase transition to uniform matter. We compare our results with thermodynamic spinodals calculated using the same Skyrme parameterizations, finding that the effect of short-range Coulomb correlations and quantum shell effects included in our model leads to the pasta phases existing at densities up to 0.1 fm −3 above the spinodal boundaries, thus increasing the transition density to uniform matter by the same amount. The transition density is otherwise shown to be insensitive to the symmetry energy at saturation density within the range constrained by the concordance of a variety of experimental constraints, and can be taken to be a well-determined quantity.

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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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Low-density instabilities in relativistic asymmetric matter of compact stars

Cited by 67 publications

References 44 publications

Equation of state and thickness of the inner crust of neutron stars

Equation of state and thickness of the inner crust of neutron stars

Phase transitions in core-collapse supernova matter at sub-saturation densities

Isospin-dependent clusterization of neutron-star matter

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