Lorentz covariant nucleon self-energy decomposition of the nuclear symmetry energy

Cai, Bao-Jun; Chen, Lie‐Wen

doi:10.1016/j.physletb.2012.03.058

Cited by 28 publications

(22 citation statements)

References 65 publications

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“…To our best knowledge, the HVH decomposition of E sym (ρ) and L based on the Lorentz-covariant nucleon self-energies in relativistic approaches was first given by Cai and Chen in ref. [180]. Similar to their non-relativistic counterparts discussed in Sect.…”

Section: The Role Of the Fock Exchange Terms In Relativistic Modelssupporting

confidence: 59%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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Section: The Role Of the Fock Exchange Terms In Relativistic Modelssupporting

confidence: 59%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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“…In contrast, an alternative decomposition based on the Lorentz-covariant forms of nucleon self-energies has been proposed in Refs. [69][70][71], and it is more consistent with the experimental analyses. In the present paper, we adopt this decomposition to clarify the density dependence of E sym and its slope parameter, L, and study the properties of dense matter in detail within RHF approximation [72,73].…”

Section: Introductionsupporting

confidence: 85%

Fock contributions to nuclear symmetry energy and its slope parameter based on Lorentz-covariant decomposition of nucleon self-energies

Miyatsu,

Cheoun,

Ishizuka

et al. 2019

Preprint

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Using relativistic Hartree-Fock (RHF) approximation, we study the effect of Fock terms on the nuclear properties not only around the saturation density, ρ 0 , but also at higher densities. In particular, we investigate how the momentum dependence due to the exchange contribution affects the nuclear symmetry energy and its slope parameter, using the Lorentz-covariant decomposition of nucleon self-energies in an extended version of the RHF model, in which the exchange terms are adjusted so as to reproduce the single-nucleon potential at ρ 0 . We find that the Fock contribution suppresses the kinetic term of nuclear symmetry energy at the densities around and beyond ρ 0 .It is noticeable that not only the isovector-vector (ρ) meson but also the isoscalar mesons (σ, ω)and pion make significant influence on the potential term of nuclear symmetry energy through the exchange diagrams. Furthermore, the exchange contribution prevents the slope parameter from increasing monotonically at high densities.

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“…[29]. In this article, the nuclear symmetry energy and its slope parameter L were decomposed in terms of the Lorentz covariant nucleon self-energies, using the HugenholtzVan Hove theorem at zero temperature.…”

Section: B Approximating the Asymmetry Dependencementioning

confidence: 99%

“…In Ref. [29], also momentum-dependent interactions and a scalar isovector interaction were considered, which are not taken into account here. However, the derivation of Ref.…”

Section: B Approximating the Asymmetry Dependencementioning

confidence: 99%

Nucleon self-energies for supernova equations of state

Hempel

2015

Phys. Rev. C

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Nucleon self-energies and interaction potentials in supernova (SN) matter, which are known to have an important effect on nucleosynthesis conditions in SN ejecta are investigated. Corresponding weak charged-current interaction rates with unbound nucleons that are consistent with existing SN equations of state (EOSs) are specified. The nucleon self-energies are made available online as electronic tables. The discussion is mostly restricted to relativistic mean-field models. In the first part of the article, the generic properties of this class of models at finite temperature and asymmetry are studied. It is found that the quadratic expansion of the EOS in terms of asymmetry works reasonably well at finite temperatures and deviations originate mostly from the kinetic part. The interaction part of the symmetry energy is found to be almost temperature independent. At low densities, the account of realistic nucleon masses requires the introduction of a linear term in the expansion. Finally, it is shown that the important neutron-to-proton potential difference is given approximately by the asymmetry of the system and the interaction part of the zero-temperature symmetry energy. The results of different interactions are then compared with constraints from nuclear experiments and thereby the possible range of the potential difference is limited. In the second part, for a certain class of SN EOS models, the formation of nuclei is considered. Only moderate modifications are found for the self-energies of unbound nucleons that enter the weak charged-current interaction rates. This is because in the present approach the binding energies of bound states do not contribute to the single-particle energies of unbound nucleons.

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Lorentz covariant nucleon self-energy decomposition of the nuclear symmetry energy

Cited by 28 publications

References 65 publications

Towards understanding astrophysical effects of nuclear symmetry energy

Towards understanding astrophysical effects of nuclear symmetry energy

Fock contributions to nuclear symmetry energy and its slope parameter based on Lorentz-covariant decomposition of nucleon self-energies

Nucleon self-energies for supernova equations of state

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