scholarly journals Density dependence of the symmetry energy from neutron skin thickness in finite nuclei

2012 ◽  
Author(s):  
X. Viñas ◽  
M. Centelles ◽  
X. Roca-Maza ◽  
M. Warda
Keyword(s):  
Density Dependence ◽  
Symmetry Energy ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Neutron Skin Thickness ◽  
Finite Nuclei

Neutron skin thickness of finite nuclei with finite range effective interaction in droplet model

2018 ◽  
Vol 27 (06) ◽  
pp. 1850049 ◽  
Author(s):  
M. Pal ◽  
S. Chakraborty ◽  
B. Sahoo ◽  
S. Sahoo
Keyword(s):  
Symmetry Energy ◽  
Effective Interaction ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Droplet Model ◽  
Density Region ◽  
Neutron Skin Thickness ◽  
Number Formula ◽  
Energy Formula ◽  
Finite Nuclei

We analyze the relation between the symmetry energy coefficient [Formula: see text] of finite nuclei with mass number [Formula: see text] in the semi-empirical mass formula. The nuclear matter symmetry energy [Formula: see text] at reference density [Formula: see text] in the subsaturation density region can be determined by the symmetry energy [Formula: see text] and its density slope [Formula: see text] at the saturation density [Formula: see text]. From this relation, the neutron skin thickness ‘[Formula: see text]’ in finite nuclei with droplet model are correlated to the various symmetry energy parameters. A prominent role of the bulk symmetry energy [Formula: see text] to the so-called surface stiffness coefficient [Formula: see text] is observed in deriving the size of the neutron skin. Two types of neutron skins are distinguished: the “surface” and the “bulk”. The linear dependence of the neutron skin thickness for different stable nuclei ([Formula: see text]) on the slope [Formula: see text] of the symmetry energy as well as on the relative neutron excess [Formula: see text] is observed. Though the value of the surface width is found to be limited within 0.1[Formula: see text]fm, its contribution should not be neglected to measure neutron skin thickness.

Effects of pairing correlations on the neutron skin thickness and the symmetry energy

2017 ◽  
Vol 96 (2) ◽  
Author(s):  
Soonchul Choi ◽  
Ying Zhang ◽  
Myung-Ki Cheoun ◽  
Youngshin Kwon ◽  
Kyungsik Kim ◽  
...  
Keyword(s):  
Symmetry Energy ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Neutron Skin Thickness ◽  
Pairing Correlations

Study of the dependence of alpha decay half-life on the surface symmetry energy

2020 ◽  
Vol 29 (09) ◽  
pp. 2050070
Author(s):  
S. Nejati ◽  
O. N. Ghodsi
Keyword(s):  
Symmetry Energy ◽  
Half Life ◽  
Surface Region ◽  
Alpha Decay ◽  
Proton Density ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Mother And Daughter ◽  
Energy Coefficient ◽  
Finite Nuclei

In this study, the effect of the surface symmetry energy on the neutron skin thickness and division of it into the bulk and surface parts are investigated by determination of the symmetry energy coefficient [Formula: see text] of finite nuclei. We demonstrate the importance of the isospin asymmetry distribution in the symmetry energy coefficient of finite nuclei at the surface region. We attempt to find out how different surface symmetry energies may affect alpha decay half-life. The Skyrme interactions are used to describe the neutron and proton density distributions and to calculate the symmetry energy coefficient [Formula: see text] of four nuclei and the surface symmetry energy. The chosen Skyrme interactions can produce the binding energy and root-mean-square charge radii of both mother and daughter nuclei. We single out the spherical isotones of [Formula: see text] named [Formula: see text]Pb, [Formula: see text]Po, [Formula: see text]Rn and [Formula: see text]Ra for daughter nuclei and explore the dependence of the bulk and surface contributions on the surface symmetry energy. The half-life of mother nuclei, i.e., [Formula: see text]Po, [Formula: see text]Rn, [Formula: see text]Ra and [Formula: see text]Th, is employed to investigate the extent to which it is affected by different surface symmetry energies. The calculated half-lives show a downward tendency for different surface symmetry energies which can be caused by various neutron skin thicknesses.

scholarly journals The Equation of State of Nuclear Matter: From Finite Nuclei to Neutron Stars

Universe ◽  
2020 ◽  
Vol 6 (8) ◽  
pp. 119 ◽  
Author(s):  
G. Fiorella Burgio ◽  
Isaac Vidaña
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Quantum Monte Carlo ◽  
Equations Of State ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Large Set ◽  
Solar Mass ◽  
Atomic Nuclei ◽  
Neutron Skin Thickness

Background. We investigate possible correlations between neutron star observables and properties of atomic nuclei. In particular, we explore how the tidal deformability of a 1.4 solar mass neutron star, M1.4, and the neutron-skin thickness of 48Ca and 208Pb are related to the stellar radius and the stiffness of the symmetry energy. Methods. We examine a large set of nuclear equations of state based on phenomenological models (Skyrme, NLWM, DDM) and ab initio theoretical methods (BBG, Dirac–Brueckner, Variational, Quantum Monte Carlo). Results: We find strong correlations between tidal deformability and NS radius, whereas a weaker correlation does exist with the stiffness of the symmetry energy. Regarding the neutron-skin thickness, weak correlations appear both with the stiffness of the symmetry energy, and the radius of a M1.4. Our results show that whereas the considered EoS are compatible with the largest masses observed up to now, only five microscopic models and four Skyrme forces are simultaneously compatible with the present constraints on L and the PREX experimental data on the 208Pb neutron-skin thickness. We find that all the NLWM and DDM models and the majority of the Skyrme forces are excluded by these two experimental constraints, and that the analysis of the data collected by the NICER mission excludes most of the NLWM considered. Conclusion. The tidal deformability of a M1.4 and the neutron-skin thickness of atomic nuclei show some degree of correlation with nuclear and astrophysical observables, which however depends on the ensemble of adopted EoS.

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