Effects of direct nucleon-nucleon interactions in pion-condensed neutron star matter

1988 ◽  
Vol 37 (4) ◽  
pp. 1711-1728 ◽  
Author(s):  
Rune Mittet ◽  
Erlend stgaard
Keyword(s):  
Neutron Star ◽  
Nucleon Nucleon ◽  
Neutron Star Matter ◽  
Nucleon Interactions

The properties of neutron star in the framework of relativistic Hartree–Fock model with unitary correlation operator method

2019 ◽  
Vol 28 (11) ◽  
pp. 1950094 ◽  
Author(s):  
Ying Zhang ◽  
Peng Liu ◽  
Jinniu Hu
Keyword(s):  
Neutron Star ◽  
Equations Of State ◽  
Operator Method ◽  
Nucleon Nucleon ◽  
Neutron Star Matter ◽  
Tensor Correlation ◽  
Correlation Operator ◽  
Hartree Fock ◽  
Unitary Correlation Operator Method ◽  
Strong Repulsion

The properties of neutron star are studied in the framework of relativistic Hartree–Fock (RHF) model with realistic nucleon–nucleon (NN) interactions, i.e., Bonn potentials. The strong repulsion of NN interaction at short range is properly removed by the unitary correlation operator method (UCOM). Meanwhile, the tensor correlation is neglected due to the very rich neutron environment in neutron star, where the total isospin of two nucleons can be approximately regarded as [Formula: see text]. The equations of state of neutron star matter are calculated in [Formula: see text] equilibrium and charge neutrality conditions. The properties of neutron star, such as mass, radius and tidal deformability, are obtained by solving the Tolman–Oppenheimer–Volkoff equation and tidal equation. The maximum masses of neutron from Bonn A, B, C potentials are around [Formula: see text]. The radius are [Formula: see text][Formula: see text]km at [Formula: see text], respectively. The corresponding tidal deformabilities are [Formula: see text]. All of these properties are satisfied with the recent observables from the astronomical and gravitational wave devices and are consistent with the results from the relativistic Brueckner–Hartree–Fock model.

PROTON SUPERFLUIDITY IN NEUTRON STAR MATTER WITH AN EFFECTIVE INTERACTION

1995 ◽  
Vol 04 (04) ◽  
pp. 843-848 ◽  
Author(s):  
G. LAZZARI ◽  
F.V. DE BLASIO
Keyword(s):  
Neutron Star ◽  
Proton Energy ◽  
Energy Gap ◽  
Effective Interaction ◽  
Nucleon Nucleon ◽  
Neutron Star Matter ◽  
Nucleon Interaction ◽  
Effective Force ◽  
Nucleon Nucleon Interaction ◽  
Considerable Range

The isotropic proton superfluidity in Neutron Star Matter is evaluated in the conventional BCS approach using Gogny effective force as the nucleon-nucleon interaction. We have found that, neglecting the polarizability effects and including different proton concentrations in neutron star matter, the 1S0 proton energy gap is considerably smaller than the corresponding neutron isotropic gap. It is shown that at higher densities proton superfluidity could prevail in a considerable range of density in the interior of a neutron star.

scholarly journals Symmetry Energy and the Pauli Exclusion Principle

Symmetry ◽  
2021 ◽  
Vol 13 (11) ◽  
pp. 2116
Author(s):  
Claudio O. Dorso ◽  
Guillermo Frank ◽  
Jorge A. López
Keyword(s):  
Neutron Star ◽  
Symmetry Energy ◽  
Pauli Exclusion Principle ◽  
Nucleon Nucleon ◽  
Binding Energies ◽  
Exclusion Principle ◽  
Neutron Star Matter ◽  
Intermediate Energies ◽  
Metropolis Monte Carlo ◽  
Finite Nuclei

In this article we present a classical potential that respects the Pauli exclusion principle and can be used to describe nucleon-nucleon interactions at intermediate energies. The potential depends on the relative momentum of the colliding nucleons and reduces interactions at low momentum transfer mimicking the Pauli exclusion principle. We use the potential with Metropolis Monte Carlo methods and study the formation of finite nuclei and infinite systems. We find good agreement in terms of the binding energies, radii, and internal nucleon distribution of finite nuclei, and the binding energy in nuclear matter and neutron star matter, as well as the formation of nuclear pastas, and the symmetry energy of neutron star matter.

scholarly journals Neutron Star Properties in the Thomas-Fermi Model

1997 ◽  
Vol 06 (04) ◽  
pp. 669-691 ◽  
Author(s):  
K. Strobel ◽  
F. Weber ◽  
Ch. Schaab ◽  
M. K. Weigel
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Optical Potential ◽  
Nucleon Nucleon ◽  
Neutron Star Matter ◽  
Fermi Model ◽  
Cooling Behavior ◽  
Nucleon Nucleon Interaction ◽  
Finite Nuclei ◽  
The Impact

The modern nucleon-nucleon interaction of Myers and Swiatecki, adjusted to the properties of finite nuclei, the parameters of the mass formula, and the behavior of the optical potential is used to calculate the properties of β-equilibrated neutron star matter, and to study the impact of this equation of state on the properties of (rapidly rotating) neutron stars and their cooling behavior. The results are in excellent agreement with the outcome of calculations performed for a broad collection of sophisticated nonrelativistic as well as relativistic models for the equation of state.

scholarly journals Transport Coefficients of Hyperonic Neutron Star Cores

Universe ◽  
2021 ◽  
Vol 7 (6) ◽  
pp. 203
Author(s):  
Peter Shternin ◽  
Isaac Vidaña
Keyword(s):  
Thermal Conductivity ◽  
Neutron Star ◽  
Shear Viscosity ◽  
Transport Coefficients ◽  
Dense Matter ◽  
Baryon Number ◽  
Nucleon Nucleon ◽  
Total Thermal Conductivity ◽  
Nucleon Force ◽  
Density Region

We consider transport properties of the hypernuclear matter in neutron star cores. In particular, we calculate the thermal conductivity, the shear viscosity, and the momentum transfer rates for npΣ−Λeμ composition of dense matter in β–equilibrium for baryon number densities in the range 0.1–1 fm−3. The calculations are based on baryon interactions treated within the framework of the non-relativistic Brueckner-Hartree-Fock theory. Bare nucleon-nucleon (NN) interactions are described by the Argonne v18 phenomenological potential supplemented with the Urbana IX three-nucleon force. Nucleon-hyperon (NY) and hyperon-hyperon (YY) interactions are based on the NSC97e and NSC97a models of the Nijmegen group. We find that the baryon contribution to transport coefficients is dominated by the neutron one as in the case of neutron star cores containing only nucleons. In particular, we find that neutrons dominate the total thermal conductivity over the whole range of densities explored and that, due to the onset of Σ− which leads to the deleptonization of the neutron star core, they dominate also the shear viscosity in the high density region, in contrast with the pure nucleonic case where the lepton contribution is always the dominant one.

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