Warm and cold pasta phase in relativistic mean field theory

Avancini, S. S.; Menezes, D. P.; Alloy, Marcelo D.; Marinelli, J. R.; Moraes, Mello; Providência, Constança

doi:10.1103/physrevc.78.015802

Cited by 142 publications

(196 citation statements)

References 32 publications

Supporting

Mentioning

185

Contrasting

Order By: Relevance

“…6, where we show the pressure of asymmetric nuclear matter evaluated at normal saturation density ρ 0 for the isospin asymmetries of 208 Pb (β = 44/208) and 132 Sn (β = 32/132). Note that, since the BHF calculation predicts larger values for ρ 0 than the other approaches (see Table I), its result appears in both cases, 208 Pb and 132 Sn, a bit out of the trends marked by the other models.Another sensitive quantity to the symmetry energy is the transition density ρ t from non-uniform to uniform β-stable matter which may be estimated from the crossing of the β-equilibrium equation of state with the thermodynamical spinodal instability line [44,[58][59][60][61][62]. As it has been shown in Ref.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Density dependence of the nuclear symmetry energy: A microscopic perspective

et al. 2009

View full text Add to dashboard Cite

We perform a systematic analysis of the density dependence of the nuclear symmetry energy within the microscopic Brueckner-Hartree-Fock (BHF) approach using the realistic Argonne V18 nucleon-nucleon potential plus a phenomenological three body force of Urbana type. Our results are compared thoroughly to those arising from several Skyrme and relativistic effective models.The values of the parameters characterizing the BHF equation of state of isospin asymmetric nuclear matter fall within the trends predicted by those models and are compatible with recent constraints coming from heavy ion collisions, giant monopole resonances or isobaric analog states.In particular we find a value of the slope parameter L = 66.9 MeV, compatible with recent experimental constraints from isospin diffusion, L = 88 ± 25 MeV. The correlation between the neutron skin thickness of neutron-rich isotopes and the slope, L, and curvature, K sym , parameters of the symmetry energy is studied. Our BHF results are in very good agreement with the correlations already predicted by other authors using non-relativistic and relativistic effective models. The correlations of these two parameters and the neutron skin thickness with the transition density from non-uniform to β-stable matter in neutron stars are also analyzed. Our results confirm that there is an inverse correlation between the neutron skin thickness and the transition density.PACS numbers: 21.65.Cd; 21.65.Ef; 21.65.Mn 2 A well-grounded understanding of the properties of isospin-rich nuclear matter is a necessary ingredient for the advancement of both nuclear physics and astrophysics. Isospin asymmetric nuclear matter is present in nuclei, especially in those far away from the stability line, and in astrophysical systems, particularly in neutron stars. A major scientific effort is being carried out at an international level to study experimentally the properties of asymmetric nuclear systems. Laboratory measurements, such as those running or planned to run in the existing or the next-generation, radioactive ion beam facilities at CSR (China), FAIR (Germany), RIKEN (Japan), SPIRAL2/GANIL (France) and the upcoming FRIB (USA), can probe the behavior of the symmetry energy close and above saturation density [1]. Moreover, the 208 Pb Radius Experiment (PREX), scheduled to run at JLab in early 2010, should provide a very accurate measurement of the neutron skin thickness in lead via parity violating electron scattering [2]. Astrophysical observations of compact objects are also a window into both the bulk and the microscopic properties of nuclear matter at extreme isospin asymmetries [3]. The symmetry energy determines to a large extent the composition of β-stable matter and therefore the structure and mass of a neutron star [4].The empirical knowledge gathered from all these sources should be helpful in identifying the major issues arising when the isospin content of nuclear systems is altered. Reliable theoretical investigations of neutron-rich (and possibly proton-rich) systems are...

show abstract

mentioning

confidence: 99%

“…Another sensitive quantity to the symmetry energy is the transition density ρ t from non-uniform to uniform β-stable matter which may be estimated from the crossing of the β-equilibrium equation of state with the thermodynamical spinodal instability line [44,[58][59][60][61][62]. As it has been shown in Ref.…”

mentioning

confidence: 99%

Density dependence of the nuclear symmetry energy: A microscopic perspective

et al. 2009

View full text Add to dashboard Cite

show abstract

“…It was shown that the main differences occur at large isospin asymmetry and at finite temperature. In particular it has been shown that the predicted density at the inner edge of the crust of a compact star, from the crossing of the β-equilibrium equation of state (EOS), is model dependent [9].…”

Section: Introductionmentioning

confidence: 99%

Low density instabilities in asymmetric nuclear matter within the quark-meson coupling (QMC) model with the δ meson

2009

View full text Add to dashboard Cite

In the present work we include the isovector-scalar δ-meson in the quark-meson coupling model (QMC) and study the properties of asymmetric nuclear within QMC without and with the δ-meson. Recent constraints set by isospin diffusion on the slope parameter of the nuclear symmetry energy at saturation density are used to adjust the model parameters. The thermodynamical spinodal surfaces are obtained and the instability region at subsaturation densities within QMC and QMCδ models are compared with mean-field relativistic models. The distillation effect in the QMC model is discussed.

show abstract

“…Approaches to the problem that do not explicitly assume any shape for the nuclear pasta have also been considered. They include calculations based on the ThomasFermi approximation [2,[12][13][14], Hartree-Fock methods [15][16][17], density-functional theory [18], relativistic mean field approximation [10,19], quantum molecular dynamics (QMD) [20][21][22][23][24][25][26] and semi-classical molecular dynamics (MD) [6,7,[27][28][29][30].…”

Section: Introductionmentioning

confidence: 99%

Nuclear “pasta” formation

et al. 2013

View full text Add to dashboard Cite

The formation of complex nonuniform phases of nuclear matter, known as nuclear pasta, is studied with molecular dynamics simulations containing 51 200 nucleons. A phenomenological nuclear interaction is used that reproduces the saturation binding energy and density of nuclear matter. Systems are prepared at an initial density of 0.10 fm −3 and then the density is decreased by expanding the simulation volume at different rates to densities of 0.01 fm −3 or less. An originally uniform system of nuclear matter is observed to form spherical bubbles ("swiss cheese"), hollow tubes, flat plates ("lasagna"), thin rods ("spaghetti") and, finally, nearly spherical nuclei with decreasing density. We explicitly observe nucleation mechanisms, with decreasing density, for these different pasta phase transitions. Topological quantities known as Minkowski functionals are obtained to characterize the pasta shapes. Different pasta shapes are observed depending on the expansion rate. This indicates non equilibrium effects. We use this to determine the best ways to obtain lower energy states of the pasta system from MD simulations and to place constrains on the equilibration time of the system.

show abstract

Warm and cold pasta phase in relativistic mean field theory

Cited by 142 publications

References 32 publications

Density dependence of the nuclear symmetry energy: A microscopic perspective

Density dependence of the nuclear symmetry energy: A microscopic perspective

Low density instabilities in asymmetric nuclear matter within the quark-meson coupling (QMC) model with the δ meson

Nuclear “pasta” formation

Contact Info

Product

Resources

About