Binding Energy of Neutron Star Matter

1972 ◽  
Vol 50 (19) ◽  
pp. 2277-2285 ◽  
Author(s):  
Dale Ellis ◽  
Donald W. L. Sprung
Keyword(s):  
Neutron Star ◽  
Binding Energy ◽  
Simple Form ◽  
Maximum Concentration ◽  
Matter Density ◽  
Matrix Elements ◽  
Neutron Star Matter ◽  
Nuclear Matter Density ◽  
Reaction Matrix ◽  
Normal Nuclear Matter Density

The energy per particle of neutron star matter is calculated using reaction matrix elements deduced from Reid's potential. These are parameterized so that the calculation is presented in a simple form. A maximum concentration of nearly 9% protons is found at about twice normal nuclear matter density.

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.

Binding energy of neutron star matter

1967 ◽  
Vol 24 (3) ◽  
pp. 137-139 ◽  
Author(s):  
J. Nemeth ◽  
D.W.L. Sprung ◽  
P.C. Bhargava
Keyword(s):  
Neutron Star ◽  
Binding Energy ◽  
Neutron Star Matter

scholarly journals A Simple Equation of State of Matter at Super-Nuclear Densities

1974 ◽  
Vol 53 ◽  
pp. 93-104
Author(s):  
Y. C. Leung ◽  
C. G. Wang
Keyword(s):  
Mass Spectrum ◽  
Neutron Star ◽  
Equation Of State ◽  
Effective Mass ◽  
Simple Form ◽  
Asymptotic Form ◽  
Matter Density ◽  
Careful Examination ◽  
Particle Interactions ◽  
State Of Matter

The qualitative features of the equation of state of matter at supernuclear densities are deduced through a careful examination of the nature of particle interactions at short distances and by the introduction of an ‘effective mass spectrum.’ it is found that the equation of state begins to take on a particularly simple form (the ‘asymptotic form’) at a relatively low matter density of 1017 g cm−3. A brief review of various approaches to calculate the equation of state for a neutron star is also given.

scholarly journals Anomalous thermodynamics and phase transitions in neutron star matter

2007 ◽  
Vol 75 (6) ◽  
Author(s):  
C. Ducoin ◽  
K. H. O. Hasnaoui ◽  
P. Napolitani ◽  
Ph. Chomaz ◽  
F. Gulminelli
Keyword(s):  
Phase Transitions ◽  
Neutron Star ◽  
Neutron Star Matter

Proton Fraction in Hot Neutron Star Matter with a Chiral Hadronic Model

2002 ◽  
Vol 19 (10) ◽  
pp. 1432-1435 ◽  
Author(s):  
Guo Hua ◽  
Zhou Ran ◽  
Liu Yu-Xin
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Hadronic Model
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