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

Ying Zhang

Department of Physics, School of Science, Tianjin University, Tianjin 300072, P. R. China

Strangeness Nuclear Physics Laboratory, RIKEN Nishina Center, Wako, 351-0198, Japan

E-mail Address: yzhangjcnp@tju.edu.cn

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Peng Liu

Tianjin Institute of Aerospace Mechanical, and Electrical Equipment, Tianjin 300301, P. R. China

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, and

Jinniu Hu

School of Physics, Nankai University, Tianjin 300071, P. R. China

Strangeness Nuclear Physics Laboratory, RIKEN Nishina Center, Wako, 351-0198, Japan

E-mail Address: hujinniu@nankai.edu.cn

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https://doi.org/10.1142/S0218301319500940Cited by:2 (Source: Crossref)

Abstract

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 $T = 1$ . The equations of state of neutron star matter are calculated in $β$ 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 $2.2 M_{⊙}$ . The radius are $12.40 - 12.91$ km at $1.4 M_{⊙}$ , respectively. The corresponding tidal deformabilities are $Λ_{1.4} = 293 - 355$ . 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.

Keywords:

PACS: 21.65.+f, 21.65.Cd, 24.10.Cn, 21.60.-n

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