摘要
The relativistic mean-field models tested in previous works against nuclear matter experimental values,critical parameters and macroscopic stellar properties are revisited and used in the evaluation of the symmetry energyγ parameter obtained in three different ways. We have checked that, independent of the choice made to calculate theγ values, a trend of linear correlation is observed between γ and the symmetry energy（S0） and a more clear linear relationship is established between γ and the slope of the symmetry energy（L0）. These results directly contribute to the arising of other linear correlations between γ and the neutron star radii of R（1.0） and R（1.4）, in agreement with recent findings. Finally, we have found that short-range correlations induce two specific parametrizations, namely,IU-FSU and DD-MEδ, simultaneously compatible with the neutron star mass constraint of 1.93≤M（max）/M☉≤2.05 and with the overlap band for the L0 ×S0 region, to present γ in the range of γ=0.25±0.05.
The relativistic mean-field models tested in previous works against nuclear matter experimental values,critical parameters and macroscopic stellar properties are revisited and used in the evaluation of the symmetry energyγ parameter obtained in three different ways. We have checked that, independent of the choice made to calculate theγ values, a trend of linear correlation is observed between γ and the symmetry energy（S0） and a more clear linear relationship is established between γ and the slope of the symmetry energy（L0）. These results directly contribute to the arising of other linear correlations between γ and the neutron star radii of R（1.0） and R（1.4）, in agreement with recent findings. Finally, we have found that short-range correlations induce two specific parametrizations, namely,IU-FSU and DD-MEδ, simultaneously compatible with the neutron star mass constraint of 1.93≤M（max）/M☉≤2.05 and with the overlap band for the L0 ×S0 region, to present γ in the range of γ=0.25±0.05.
基金
a part of the project INCT-FNA Proc.No.464898/2014-5
partially supported by Conselho Nacional de Desenvolvimento Científico e Tecnológico(CNPq)
Brazil under grants 300602/2009-0 and 306786/2014-1
support from the Israel Science Foundation
the U.S.Department of Energy Office of Science,Office of Nuclear Physics program under award number DE-FG02-94ER40818
