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Title: Dynamical properties of nuclear and stellar matter and the symmetry energy

Abstract

The effects of density dependence of the symmetry energy on the collective modes and dynamical instabilities of cold and warm nuclear and stellar matter are studied in the framework of relativistic mean-field hadron models. The existence of the collective isovector and possibly an isoscalar collective mode above saturation density is discussed. It is shown that soft equations of state do not allow for a high-density isoscalar collective mode; however, if the symmetry energy is hard enough, an isovector mode will not disappear at high densities. The crust-core transition density and pressure are obtained as a function of temperature for {beta}-equilibrium matter with and without neutrino trapping. Estimations of the size of the clusters formed in the nonhomogeneous phase, as well as the corresponding growth rates and distillation effect, are made. It is shown that cluster sizes increase with temperature, that the distillation effect close to the inner edge of the crust-core transition is very sensitive to the symmetry energy, and that, within a dynamical instability calculation, the pasta phase exists in warm compact stars up to 10-12 MeV.

Authors:
; ; ;  [1]
  1. Centro de Fisica Computacional, Department of Physics, University of Coimbra, P-3004-516 Coimbra (Portugal)
Publication Date:
OSTI Identifier:
21419468
Resource Type:
Journal Article
Journal Name:
Physical Review. C, Nuclear Physics
Additional Journal Information:
Journal Volume: 82; Journal Issue: 2; Other Information: DOI: 10.1103/PhysRevC.82.025801; (c) 2010 The American Physical Society; Journal ID: ISSN 0556-2813
Country of Publication:
United States
Language:
English
Subject:
73 NUCLEAR PHYSICS AND RADIATION PHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; DENSITY; DISTILLATION; EQUATIONS OF STATE; EQUILIBRIUM; HADRONS; INSTABILITY; ISOVECTORS; MEAN-FIELD THEORY; MEV RANGE 10-100; NEUTRINOS; NUCLEAR MATTER; RELATIVISTIC RANGE; SATURATION; STARS; SYMMETRY; TEMPERATURE DEPENDENCE; TRAPPING; ELEMENTARY PARTICLES; ENERGY RANGE; EQUATIONS; FERMIONS; LEPTONS; MASSLESS PARTICLES; MATTER; MEV RANGE; PHYSICAL PROPERTIES; SEPARATION PROCESSES; TENSORS; VECTORS

Citation Formats

Pais, Helena, Santos, Alexandre, Brito, Lucilia, and Providencia, Constanca. Dynamical properties of nuclear and stellar matter and the symmetry energy. United States: N. p., 2010. Web. doi:10.1103/PHYSREVC.82.025801.
Pais, Helena, Santos, Alexandre, Brito, Lucilia, & Providencia, Constanca. Dynamical properties of nuclear and stellar matter and the symmetry energy. United States. https://doi.org/10.1103/PHYSREVC.82.025801
Pais, Helena, Santos, Alexandre, Brito, Lucilia, and Providencia, Constanca. 2010. "Dynamical properties of nuclear and stellar matter and the symmetry energy". United States. https://doi.org/10.1103/PHYSREVC.82.025801.
@article{osti_21419468,
title = {Dynamical properties of nuclear and stellar matter and the symmetry energy},
author = {Pais, Helena and Santos, Alexandre and Brito, Lucilia and Providencia, Constanca},
abstractNote = {The effects of density dependence of the symmetry energy on the collective modes and dynamical instabilities of cold and warm nuclear and stellar matter are studied in the framework of relativistic mean-field hadron models. The existence of the collective isovector and possibly an isoscalar collective mode above saturation density is discussed. It is shown that soft equations of state do not allow for a high-density isoscalar collective mode; however, if the symmetry energy is hard enough, an isovector mode will not disappear at high densities. The crust-core transition density and pressure are obtained as a function of temperature for {beta}-equilibrium matter with and without neutrino trapping. Estimations of the size of the clusters formed in the nonhomogeneous phase, as well as the corresponding growth rates and distillation effect, are made. It is shown that cluster sizes increase with temperature, that the distillation effect close to the inner edge of the crust-core transition is very sensitive to the symmetry energy, and that, within a dynamical instability calculation, the pasta phase exists in warm compact stars up to 10-12 MeV.},
doi = {10.1103/PHYSREVC.82.025801},
url = {https://www.osti.gov/biblio/21419468}, journal = {Physical Review. C, Nuclear Physics},
issn = {0556-2813},
number = 2,
volume = 82,
place = {United States},
year = {Sun Aug 15 00:00:00 EDT 2010},
month = {Sun Aug 15 00:00:00 EDT 2010}
}