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.

scholarly journals Symmetrie and Asymmetrie Nuclear Matter in the Thomas-Fermi Model at Finite Temperatures

1999 ◽  
Vol 54 (1) ◽  
pp. 83-90 ◽  
Author(s):  
K. Strobel ◽  
F. Weber ◽  
M. K. Weigel
Keyword(s):  
Nuclear Matter ◽  
Gas Phase ◽  
Nuclear Physics ◽  
Cold Neutron ◽  
Critical Density ◽  
Nucleon Nucleon ◽  
Neutron Star Matter ◽  
Fermi Model ◽  
Thomas Fermi ◽  
Nucleon Nucleon Interaction

Abstract The properties of warm symmetric and asymmetric nuclear matter are investigated in the frame of the Thomas-Fermi approximation using a recent modern parameterization of the effective nucleon-nucleon interaction of Myers and Świątecki. Special attention is paid to the liquid-gas phase transition, which is of special interest in modern nuclear physics. We have determined the critical temperature, critical density and the so-called flash temperature. Furthermore, the equation of state for cold neutron star matter is calculated.

ON COMPRESSED NUCLEAR MATTER: FROM NUCLEI TO NEUTRON STARS

2011 ◽  
Vol 20 (10) ◽  
pp. 1789-1796 ◽  
Author(s):  
JORGE A. RUEDA ◽  
M. ROTONDO ◽  
R. RUFFINI ◽  
S.-S. XUE
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
White Dwarfs ◽  
Traditional Approach ◽  
Equilibrium Equations ◽  
Fermi Model ◽  
Thomas Fermi ◽  
General Relativistic ◽  
The Way

We address the description of neutron-proton-electron degenerate matter in beta equilibrium subjected to compression both in the case of confined nucleons into a nucleus as well as in the case of deconfined nucleons. We follow a step-by-step generalization of the classical Thomas–Fermi model to special and general relativistic regimes, which leads to a unified treatment of beta equilibrated neutron-proton-electron degenerate matter applicable from the case of nuclei all the way up to the case of white-dwarfs and neutron stars. New gravito-electrodynamical effects, missed in the traditional approach for the description of neutron star configurations, are found as a consequence of the new set of general relativistic equilibrium equations.

ON GRAVITATIONALLY AND ELECTRODYNAMICALLY BOUND NUCLEAR MATTER CORES OF STELLAR DIMENSIONS

2011 ◽  
Vol 20 (10) ◽  
pp. 1995-2002 ◽  
Author(s):  
MICHAEL ROTONDO ◽  
REMO RUFFINI ◽  
SHE-SHENG XUE ◽  
VLADIMIR POPOV
Keyword(s):  
Electric Field ◽  
Nuclear Matter ◽  
Analytic Solutions ◽  
Physical Parameters ◽  
Heavy Nuclei ◽  
Neutral Atoms ◽  
Charge Neutrality ◽  
Thomas Fermi ◽  
Surface Energies ◽  
The Stability

In a unified treatment we extrapolate results for neutral atoms with heavy nuclei to nuclear matter cores of stellar dimensions with mass numbers A ≈ (m Planck /mn)3 ~ 1057. We give explicit analytic solutions for the relativistic Thomas–Fermi equation of Nn neutrons, Np protons and Ne electrons in beta equilibrium, fulfilling global charge neutrality, with Np = Ne. We give explicit expressions for the physical parameters including the Coulomb and the surface energies and we study as well the stability of such configurations. Analogous to heavy nuclei these macroscopic cores exhibit an overcritical electric field near their surface.

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.

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