Energy per Particle of Neutron Matter near Nuclear Density

1971 ◽  
Vol 3 (4) ◽  
pp. 1487-1491 ◽  
Author(s):  
Sara L. Schlenker ◽  
E. L. Lomon
Keyword(s):  
Neutron Matter ◽  
Nuclear Density

Nuclear Density Distribution Feature for Improving Cervical Histopathological Images Recognition

2021 ◽  
Author(s):  
Zhuangzhuang Wang ◽  
Mengning Yang ◽  
Yangfan Lyu ◽  
Kairun Chen ◽  
Qicheng Tang
Keyword(s):  
Density Distribution ◽  
Nuclear Density ◽  
Histopathological Images ◽  
Images Recognition

scholarly journals Superfluid Phonons in Neutron Star Core

Universe ◽  
2021 ◽  
Vol 7 (1) ◽  
pp. 16
Author(s):  
Marcello Baldo
Keyword(s):  
Neutron Star ◽  
Inner Core ◽  
Mutual Influence ◽  
Collective Excitation ◽  
Neutron Matter ◽  
Superfluid Phase ◽  
S Wave ◽  
Spectral Functions ◽  
Open Problems ◽  
Linear Spectrum

In neutron stars the nuclear asymmetric matter is expected to undergo phase transitions to a superfluid state. According to simple estimates, neutron matter in the inner crust and just below should be in the s-wave superfluid phase, corresponding to the neutron-neutron 1S0 channel. At higher density in the core also the proton component should be superfluid, while in the inner core the neutron matter can be in the 3P2 superfluid phase. Superluidity is believed to be at the basis of the glitches phenomenon and to play a decisive influence on many processes like transport, neutrino emission and cooling, and so on. One of the peculiarity of the superfluid phase is the presence of characteristic collective excitation, the so called ’phonons’, that correspond to smooth modulations of the order parameter and display a linear spectrum at low enough momentum. This paper is a brief review of the different phonons that can appear in Neutron Star superfuid matter and their role in several dynamical processes. Particular emphasis is put on the spectral functions of the different components, that is neutron, protons and electrons, which reveal their mutual influence. The open problems are discussed and indications on the work that remain to be done are given.

Ferromagnetism in neutron matter and its implication for the neutron star equation of state

2011 ◽  
Author(s):  
J. P. W. Diener ◽  
F. G. Scholtz ◽  
Ersin Göğüş ◽  
Ünal Ertan ◽  
Tomaso Belloni
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Matter

VMC CALCULATIONS OF THE GROUND STATE PROPERTIES OF NUCLEAR MATTER

2005 ◽  
Vol 14 (02) ◽  
pp. 255-267 ◽  
Author(s):  
KAAN MANİSA ◽  
ÜLFET ATAV ◽  
RIZA OGUL
Keyword(s):  
Nuclear Matter ◽  
Ground State ◽  
Nucleon Nucleon ◽  
Neutron Matter ◽  
Potential Term ◽  
Ground State Properties ◽  
Dependent Potential ◽  
Variational Monte Carlo Method ◽  
Kinetic And Potential Energies ◽  
Good Agreement

A Variational Monte Carlo method (VMC) is described for the evaluation of the ground state properties of nuclear matter. Equilibrium properties of symmetric nuclear matter and neutron matter are calculated by the described VMC method. The Urbana ν14 potential is used for the nucleon–nucleon interactions in the calculations. Three- and more-body interactions are included as a density dependent potential term. Total, kinetic and potential energies per particle are obtained for nuclear and neutron matter. Pressure values of nuclear and neutron matter are also calculated at various densities. The binding energy of nuclear matter is found to be -16.06 MeV at a saturation density of 0.16 fm -3. The results obtained are in good agreement with those obtained by various authors with different potentials and techniques.

scholarly journals Quantum Monte Carlo calculations of neutron matter

2003 ◽  
Vol 68 (2) ◽  
Author(s):  
J. Carlson ◽  
J. Morales ◽  
V. R. Pandharipande ◽  
D. G. Ravenhall
Keyword(s):  
Monte Carlo ◽  
Quantum Monte Carlo ◽  
Neutron Matter ◽  
Monte Carlo Calculations

Superfluidity of neutron matter

1985 ◽  
Vol 437 (2) ◽  
pp. 487-508 ◽  
Author(s):  
L. Amundsen ◽  
E. Østgaard
Keyword(s):  
Neutron Matter
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