Nucleon Superfluidity in Asymmetric Nuclear Matter and Neutron Star Matter

2010 ◽  
Author(s):  
Wei Zuo ◽  
U. Lombardo ◽  
Akira Ozawa ◽  
Weiping Lu
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Neutron Star Matter ◽  
Asymmetric Nuclear Matter ◽  
Nucleon Superfluidity

scholarly journals Asymmetric Nuclear Matter and Neutron Star Properties

1996 ◽  
Vol 469 ◽  
pp. 794 ◽  
Author(s):  
L. Engvik ◽  
E. Osnes ◽  
M. Hjorth-Jensen ◽  
G. Bao ◽  
E. Ostgaard
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Asymmetric Nuclear Matter

EFFECTS OF IN-MEDIUM MODIFICATION OF WEAKLY INTERACTING LIGHT BOSON MASS IN NEUTRON STARS

2011 ◽  
Vol 26 (05) ◽  
pp. 367-375 ◽  
Author(s):  
A. SULAKSONO ◽  
MARLIANA ◽  
KASMUDIN
Keyword(s):  
Neutron Star ◽  
Binding Energy ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Observational Data ◽  
Boson Mass ◽  
Characteristic Scale ◽  
Neutron Star Matter ◽  
Weakly Interacting ◽  
Medium Modification

The effects of the presence of weakly interacting light boson (WILB) in neutron star matter have been revisited. Direct checking based on the experimental range of symmetric nuclear matter binding energy1 and the fact that the presence of this boson should give no observed effect on the crust properties of neutron star matter, shows that the characteristic scale of WILB [Formula: see text] should be ≤2 GeV-2. The recent observational data with significant low neutron stars radii2 and the recent largest pulsar which has been precisely measured, i.e. J1903+0327 (Ref. 3) indicate that in-medium modification of WILB mass in neutron stars cannot be neglected.

scholarly journals Properties and Synthesis of Heavy Nuclei and Properties of Neutron Star Matter

1974 ◽  
Vol 53 ◽  
pp. 67-75
Author(s):  
J. Robert Buchler
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Superheavy Nuclei ◽  
Heavy Nuclei ◽  
Neutron Star Matter ◽  
Fermi Model ◽  
Bulk Properties ◽  
Properties Of Nuclei ◽  
Thomas Fermi

The nuclear Thomas-Fermi model which is based on nuclear matter calculations has been successfully applied to the study of the bulk properties of nuclei. It is ideally suited for extrapolation into the region of very neutron-rich and of superheavy nuclei. It is therefore a valuable approach for r-process calculations as well as for the study of neutron star matter at subnuclear densities.

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