scholarly journals Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas. XII. Stiffness and stability of neutron-star matter

2010 ◽  
Vol 82 (3) ◽  
Author(s):  
S. Goriely ◽  
N. Chamel ◽  
J. M. Pearson
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Hartree Fock ◽  
Mass Formulas

Hartree-Fock-Bogoliubov mass formulas and the equation of state of neutron-star matter

2005 ◽  
Vol 758 ◽  
pp. 651-654 ◽  
Author(s):  
J.M. Pearson ◽  
M. Onsi ◽  
S. Goriely ◽  
M. Samyn
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Star Matter ◽  
Hartree Fock ◽  
Mass Formulas

scholarly journals A hybrid model of Skyrme- and Brueckner-type interactions for neutron star matter

2020 ◽  
Vol 2020 (1) ◽  
Author(s):  
Soonchul Choi ◽  
Myung-Ki Cheoun ◽  
K S Kim ◽  
Hungchong Kim ◽  
H Sagawa
Keyword(s):  
Neutron Star ◽  
Hybrid Model ◽  
Clear Understanding ◽  
Neutron Skin ◽  
Neutron Star Matter ◽  
Many Body ◽  
Hartree Fock ◽  
Nuclear Incompressibility ◽  
The Many ◽  
Many Body Interactions

Abstract We suggest a hybrid model for neutron star matter to discuss the hyperon puzzle inherent in the 2.0 M$_{\odot}$ of the neutron star. For the nucleon–nucleon ($NN$) interaction, we employ the Skyrme–Hartree–Fock approach based on various Skyrme interaction parameter sets, and take the Brueckner–Hartree–Fock approach for the interactions related to hyperons. For the many-body interactions including hyperons, we make use of the multi-pomeron-exchange model, whose parameters have been adjusted to the data deduced from various hypernuclei properties. For clear understanding of the physics in the hybrid model, we discuss fractional functions of related particles, symmetry energies, and chemical potentials in dense matter. Finally, we investigate the equations of state and mass–radius relation of neutron stars, and show that the hybrid model can properly describe the 2.0 M$_{\odot}$ neutron star mass data with the many-body interaction employed in the hybrid model. Recent tidal deformability data from the gravitational wave observation are also compared to our calculations, especially in terms of the neutron skin of $^{208}$Pb and nuclear incompressibility.

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.

scholarly journals Neutron Star Properties with Relativistic Equations of State

1998 ◽  
Vol 07 (03) ◽  
pp. 301-339 ◽  
Author(s):  
H. Huber ◽  
F. Weber ◽  
M. K. Weigel ◽  
Ch. Schaab
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Equations Of State ◽  
Neutron Star Matter ◽  
Hartree Fock ◽  
Standard Neutron ◽  
Relativistic Equations

We study the properties of neutron stars adopting relativistic equations of state of neutron star matter, calculated in the framework of the relativistic Brueckner–Hartree–Fock approximation for electrically charge neutral neutron star matter in beta–equilibrium. For higher densities more baryons (hyperons etc.) are included by means of the relativistic Hartree– or Hartree–Fock approximation. The special features of the different approximations and compositions are discussed in detail. Besides standard neutron star properties special emphasis is put on the limiting periods of neutron stars, for which the Kepler criterion and gravitation–reaction instabilities are considered. Furthermore the cooling behaviour of neutron stars is investigated, too. For comparison we also give the outcome for some nonrelativistic equations of state.

Effects of tensor couplings of ω and ρ mesons on 1S0 nucleon superfluidity in neutron star matter

2016 ◽  
Vol 25 (05) ◽  
pp. 1650059 ◽  
Author(s):  
Xiu-Lin Huang ◽  
Yan Xu ◽  
Cheng-Zhi Liu ◽  
Guang-Zhou Liu
Keyword(s):  
Neutron Star ◽  
Density Range ◽  
Neutron Star Matter ◽  
Hartree Fock ◽  
Relativistic Formula ◽  
Text Model ◽  
Nucleon Superfluidity

The [Formula: see text] nucleon superfluidity in neutron star matter was investigated in the framework of relativistic [Formula: see text] model with the tensor couplings of [Formula: see text] and [Formula: see text] mesons using the relativistic Hartree–Fock (RHF) approximation. It was found that the tensor couplings of [Formula: see text] and [Formula: see text] mesons lead to a clear growth of the [Formula: see text] neutron pairing gap in the density range where there exists [Formula: see text] neutron superfluidity. The [Formula: see text] pairing gap of proton with the tensor couplings of [Formula: see text] and [Formula: see text] mesons in the density range of [Formula: see text]–[Formula: see text][Formula: see text]fm[Formula: see text] is lower and then in the density range of [Formula: see text]–[Formula: see text][Formula: see text]fm[Formula: see text] higher than the corresponding value without the tensor couplings of [Formula: see text] and [Formula: see text] mesons. Our results provide a basic to understand the influence of the tensor couplings of [Formula: see text] and [Formula: see text] mesons on the cooling properties of neutron star.

scholarly journals Compatibility of Neutron Star Masses and Hyperon Coupling Constants

1999 ◽  
Vol 54 (1) ◽  
pp. 77-82 ◽  
Author(s):  
H. Huber ◽  
M. K. Weigel ◽  
F. Weber
Keyword(s):  
Neutron Star ◽  
Lower Bound ◽  
Nuclear Matter ◽  
Satisfactory Agreement ◽  
Equations Of State ◽  
Binding Energies ◽  
Coupling Constants ◽  
Neutron Star Matter ◽  
Hartree Fock ◽  
Neutron Star Mass

Abstract It is shown that the modern equations of state for neutron star matter based on microscopic calculations of symmetric and asymmetric nuclear matter are compatible with the lower bound on the maximum neutron-star mass for a certain range of hyperon coupling constants, which are constrained by the binding energies of hyperons in symmetric nuclear matter. The hyperons are included by means of the relativistic Hartree-or Hartree-Fock approximation. The obtained couplings are also in satisfactory agreement with hypernuclei data in the relativistic Hartree scheme. Within the relativistic Hartree-Fock approximation, hypernuclei have not been investigated so far.

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