NEUTRON SKIN THICKNESS AND NEUTRON STARS WITHIN A DENSITY DEPENDENT HADRONIC MODEL

2007 ◽  
Vol 16 (09) ◽  
pp. 2989-2992 ◽  
Author(s):  
S. S. AVANCINI ◽  
J. R. MARINELLI ◽  
D. P. MENEZES ◽  
M. M. W. DE MORAES ◽  
C. PROVIDÊNCIA
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Skin Thickness ◽  
Neutron Density ◽  
Neutron Skin ◽  
Density Profiles ◽  
Density Dependent ◽  
Neutron Skin Thickness ◽  
Walecka Model ◽  
Hadronic Model

A density dependent hadronic model and a common parametrization of the nonlinear Walecka model are used to obtain the lead neutron skin thickness through its proton and neutron density profiles. Our results are obtained within the Thomas–Fermi approximation. The neutron skin thickness is known to reflect the equation of state properties.

scholarly journals Density dependent hadronic models and the relation between neutron stars and neutron skin thickness

2007 ◽  
Vol 75 (5) ◽  
Author(s):  
S. S. Avancini ◽  
J. R. Marinelli ◽  
D. P. Menezes ◽  
M. M. W. Moraes ◽  
C. Providência
Keyword(s):  
Neutron Stars ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Density Dependent ◽  
Neutron Skin Thickness

scholarly journals Reexamining the neutron skin thickness within a density dependent hadronic model

2007 ◽  
Vol 76 (6) ◽  
Author(s):  
S. S. Avancini ◽  
J. R. Marinelli ◽  
D. P. Menezes ◽  
M. M. W. Moraes ◽  
A. S. Schneider
Keyword(s):  
Skin Thickness ◽  
Neutron Skin ◽  
Density Dependent ◽  
Neutron Skin Thickness ◽  
Hadronic Model

ISOSPIN EFFECT AND ISOSCALING PHENOMENON IN PROJECTILE FRAGMENTATION

2008 ◽  
Vol 17 (09) ◽  
pp. 1669-1680 ◽  
Author(s):  
C. W. MA ◽  
Y. FU ◽  
D. Q. FANG ◽  
Y. G. MA ◽  
X. Z. CAI ◽  
...  
Keyword(s):  
Excitation Energy ◽  
Projectile Fragmentation ◽  
Skin Thickness ◽  
Neutron Density ◽  
Neutron Skin ◽  
Density Distributions ◽  
Neutron Rich Nucleus ◽  
Neutron Skin Thickness ◽  
Neutron Density Distribution ◽  
The Relationship

We have studied the isospin effect and isoscaling behavior in projectile fragmentation using a modified statistical abrasion-ablation (SAA) model. The relationship between neutron skin thickness (δnp) and neutron abrasion cross section (σ nabr ) has also been investigated. We find the normalized peak differences and reduced isoscaling parameters decrease with (Z proj - Z)/Z proj or the excitation energy per nucleon and have no significant dependence on the size of the reaction systems. The excitation energy dependence of the symmetry energy coefficients are tentatively extracted from α and β. Assuming Fermi-type density distributions for proton and neutron and introducing a parameter to adjust the diffuseness of the neutron density distribution for neutron-rich nucleus, δnp and σ nabr for neutron-rich nucleus were found to have a linear correlation. It is suggested that σ nabr could be used as an observable to extract the neutron skin thickness for neutron-rich nucleus.

scholarly journals Neutron density distribution and neutron skin thickness ofPb208

2014 ◽  
Vol 90 (2) ◽  
Author(s):  
Andrea Meucci ◽  
Matteo Vorabbi ◽  
Carlotta Giusti ◽  
Paolo Finelli
Keyword(s):  
Density Distribution ◽  
Skin Thickness ◽  
Neutron Density ◽  
Neutron Skin ◽  
Neutron Skin Thickness ◽  
Neutron Density Distribution

Formation of α clusters in dilute neutron-rich matter

Science ◽  
2021 ◽  
Vol 371 (6526) ◽  
pp. 260-264 ◽  
Author(s):  
Junki Tanaka ◽  
Zaihong Yang ◽  
Stefan Typel ◽  
Satoshi Adachi ◽  
Shiwei Bai ◽  
...  
Keyword(s):  
Cross Sections ◽  
Cluster Formation ◽  
Reaction Cross ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Heavy Nuclei ◽  
Α Decay ◽  
Neutron Skin Thickness ◽  
Reaction Cross Sections ◽  
Α Particles

The surface of neutron-rich heavy nuclei, with a neutron skin created by excess neutrons, provides an important terrestrial model system to study dilute neutron-rich matter. By using quasi-free α cluster–knockout reactions, we obtained direct experimental evidence for the formation of α clusters at the surface of neutron-rich tin isotopes. The observed monotonous decrease of the reaction cross sections with increasing mass number, in excellent agreement with the theoretical prediction, implies a tight interplay between α-cluster formation and the neutron skin. This result, in turn, calls for a revision of the correlation between the neutron-skin thickness and the density dependence of the symmetry energy, which is essential for understanding neutron stars. Our result also provides a natural explanation for the origin of α particles in α decay.

Dependence of n/p with neutron skin thickness for neutron-rich nuclei

2010 ◽  
Vol 834 (1-4) ◽  
pp. 502c-504c ◽  
Author(s):  
X.Y. Sun ◽  
D.Q. Fang ◽  
Y.G. Ma ◽  
X.Z. Cai ◽  
X.G. Cao ◽  
...  
Keyword(s):  
Skin Thickness ◽  
Neutron Skin ◽  
Neutron Skin Thickness
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