Time dependence of isotopic temperatures

Barrañón, Armando; Dorso, C. O.; López, Jörge A.

doi:10.1016/j.nuclphysa.2007.04.008

Cited by 24 publications

(25 citation statements)

References 39 publications

(51 reference statements)

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“…Such potential mimics infinite systems with realistic binding energy, density and compressibility and to produce heavy-ion dynamics comparable to those predicted by the Vlasov-Nordheim equation. This parameter-free model has been successfully used to study nuclear reactions obtaining mass multiplicities, momenta, excitation energies, secondary decay yields, critical phenomena and isoscaling behavior that have been compared to experimental data [26,[67][68][69][70][71][72][73][74][75]. More recently, and of interest to the present work, the model was used to study infinite nuclear systems at low temperatures [41] and in neutron star crust environments, including the pasta structures that form in NM and NSM [10,18,19,21,32,51].…”

Section: A Classical Molecular Dynamicsmentioning

confidence: 99%

Properties of nuclear pastas

2020

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In this Review we study the nuclear pastas as they are expected to be formed in neutron star cores. We start with a study of the pastas formed in nuclear matter (composed of protons and neutrons), we follow with the role of the electron gas on the formation of pastas, and we then investigate the pastas in neutron star matter (nuclear matter embedded in an electron gas). Nuclear matter (NM) at intermediate temperatures (1 MeVT 15 MeV), at saturation and sub-saturation densities, and with proton content ranging from 30% to 50% was found to have liquid, gaseous and liquid-gas mixed phases. The isospin-dependent phase diagram was obtained along with the critical points, and the symmetry energy was calculated and compared to experimental data and other theories. At low temperatures (T 1 MeV) NM produces crystal-like structures around saturation densities, and pasta-like structures at sub-saturation densities. Properties of the pasta structures were studied with cluster-recognition algorithms, caloric curve, the radial distribution function, the Lindemann coefficient, Kolmogorov statistics, Minkowski functionals; the symmetry energy of the pasta showed a connection with its morphology.Neutron star matter (NSM) is nuclear matter embedded in an electron gas. The electron gas is included in the calculation by the inclusion of an screened Coulomb potential. To connect the NM pastas with those in neutron star matter (NSM), the role the strength and screening length of the Coulomb interaction have on the formation of the pastas in NM was investigated. Past was found to exist even without the presence of the electron gas, but the effect of the Coulomb interaction is to form more defined pasta structures, among other effects. Likewise, it was determined that there is a minimal screening length for the developed structures to be independent of the cell size.Neutron star matter was found to have similar phases as NM, phase transitions, symmetry energy, structure function and thermal conductivity. Like in NM, pasta forms at around T ≈ 1.5 MeV, and liquid-to-solid phase changes were detected at T ≈ 0.5 MeV. The structure function and the symmetry energy were also found to depend on the pasta structures. Contents I. IntroductionA. The pasta B. The pasta in nuclear matter and in neutron star matter II. Nuclear matter A. Nuclear matter at intermediate temperatures B. Nuclear matter at low temperatures C. Summary of nuclear matter properties III. Electron gas: connecting nuclear matter with neutron star matter A. The strength of V C B. The screening length C. Summarizing the electron gas IV. Neutron star matter A. Symmetric neutron star matter B. Non-symmetric neutron star matter C. The symmetry energy D. Neutrino transport properties E. Properties of non-traditional pasta F. The nucleon thermal conductivity G. Summary of NSM properties V. Conclusion A. Nuclear matter B. The electron gas C. The pasta in neutron star matter VI. Appendices A. Classical Molecular Dynamics B. The Maxwell construction C. Nuclear symmetry energy from CMD at...

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Section: A Classical Molecular Dynamicsmentioning

confidence: 99%

Properties of nuclear pastas

2020

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“…For the sake of brevity, readers interested in learning about the virtues of CMD and its comparison to other methods are directed to a previous study [8]. Here we simply reiterate that CMD has been used since 2001 [9][10][11][12][13][14][15][16] to study reactions, critical phenomena, neutron-rich nuclei (isoscaling and neutron star crusts) and, of course, phase changes and clusterization, all without any adjustable parameters. Although lacking Pauli blocking and wave dynamics, Ref.…”

Section: Classical Molecular Dynamicsmentioning

confidence: 99%

Symmetry energy in the liquid–gas mixture

López

Porras

2017

Nuclear Physics A

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Results from classical molecular dynamics simulations of infinite nuclear systems with varying density, temperature and isospin content are used to calculate the symmetry energy at low densities. The results show an excellent agreement with the experimental data and corroborate the claim that the formation of clusters has a strong influence on the symmetry energy in the liquid-gas coexistence region.

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“…This parameter-free model has been successfully used to study nuclear reactions obtaining mass multiplicities, momenta, excitation energies, secondary decay yields, critical phenomena and isoscaling behavior that have been compared to experimental data [48][49][50][51][52][53][54][55][56][57]. More recently, and of interest to the present work, the model was used to study infinite nuclear systems at low temperatures [58] and in neutron star crust environments [45][46][47].…”

Section: Classical Molecular Dynamicsmentioning

confidence: 99%

Isospin-asymmetric nuclear matter

et al. 2014

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This study uses classical molecular dynamics to simulate infinite nuclear matter and study the effect of isospin asymmetry on bulk properties such as energy per nucleon, pressure, saturation density, compressibility and symmetry energy. The simulations are performed on systems embedded in periodic boundary conditions with densities and temperatures in the ranges ρ = 0.02 to 0.2 f m −3 and T = 1, 2, 3, 4 and 5 MeV, and with isospin content of x = Z/A = 0.3, 0.4 and 0.5. The results indicate that symmetric and asymmetric matter are self-bound at some temperatures and exhibit phase transitions from a liquid phase to a liquid-gas mixture. The main effect of isospin asymmetry is found to be a reduction of the equilibrium densities, a softening of the compressibility and a disappearance of the liquid-gas phase transition. A procedure leading to the evaluation of the symmetry energy and its variation with the temperature was devised, implemented and compared to mean field theory results.

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Time dependence of isotopic temperatures

Cited by 24 publications

References 39 publications

Properties of nuclear pastas

Properties of nuclear pastas

Symmetry energy in the liquid–gas mixture

Isospin-asymmetric nuclear matter

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