Pseudo-spin symmetry in density-dependent relativistic Hartree–Fock theory

Long, Wen Hui; Sagawa, H.; Meng, J.; Giai, Nguyen Van

doi:10.1016/j.physletb.2006.05.065

Cited by 79 publications

(104 citation statements)

References 29 publications

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“…The exchange terms further lead to contributions from the pion, which are absent in the mean-field (Hartree) treatment of an infinite, spin-saturated medium due to parity conservation. A density-dependent RHF approach has recently also been developed [188][189][190], and it can describe the properties of finite nuclei and nuclear matter comparable to those in standard RMF models. As an extension of the RMF model to include the quark degree of freedom, the quark-meson coupling (QMC) model, in which quarks in non-overlapping nucleon bags interact self-consistently with (structureless) isoscalar-scalar (σ) and isoscalar-vector (ω) mesons in the mean-field approximation, has been developed [191].…”

Section: The Phenomenological Approachmentioning

confidence: 99%

“…Recently, there have been some developments in the density-dependent RHF approach [188][189][190] which can describe the properties of both finite nuclei and nuclear matter with results comparable to those from standard RMF models. A more phenomenological way to improve the results of RMF models is to introduce momentumas well as isospin-dependent form factors in the meson-nucleon coupling constants.…”

Section: Outlooksmentioning

confidence: 99%

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Recent progress and new challenges in isospin physics with heavy-ion reactions

2008

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The ultimate goal of studying isospin physics via heavy-ion reactions with neutron-rich, stable and/or radioactive nuclei is to explore the isospin dependence of in-medium nuclear effective interactions and the equation of state of neutron-rich nuclear matter, particularly the isospin-dependent term in the equation of state, i.e., the density dependence of the symmetry energy. Because of its great importance for understanding many phenomena in both nuclear physics and astrophysics, the study of the density dependence of the nuclear symmetry energy has been the main focus of the intermediate-energy heavy-ion physics community during the last decade, and significant progress has been achieved both experimentally and theoretically. In particular, a number of phenomena or observables have been identified as sensitive probes to the density dependence of the nuclear symmetry energy. Experimental studies have confirmed some of these interesting isospin-dependent effects and allowed us to constrain relatively stringently the symmetry energy at sub-saturation densities. The impacts of this constrained density dependence of the symmetry energy on the properties of neutron stars have also been studied, and they were found to be very useful for the astrophysical community. With new opportunities provided by the various radioactive beam facilities being constructed around the world, the study of isospin physics is expected to remain one of the forefront research areas in nuclear physics. In this report, we review the major progress achieved during the last decade in isospin physics with heavy ion reactions and discuss future challenges to the most important issues in this field.Key words: Equation of state of asymmetric nuclear matter, Nuclear symmetry energy, Heavy-ion reactions with neutron-rich nuclei, Neutron skin thickness of heavy nuclei, Neutron stars Constraining the Skyrme effective interactions and the neutron skin thickness of heavy nuclei using terrestrial nuclear laboratory data 216 8

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Section: The Phenomenological Approachmentioning

confidence: 99%

Section: Outlooksmentioning

confidence: 99%

Recent progress and new challenges in isospin physics with heavy-ion reactions

2008

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“…In addition, the inclusion of Fock terms has brought substantial improvements in the self-consistent description of nuclear shell structures [24] and the evolutions [25,26], the relativistic symmetry restorations [24,27,28], and the low-energy excitation modes [29].…”

Section: Introductionmentioning

confidence: 99%

Description of carbon isotopes within relativistic Hartree-Fock-Bogoliubov theory

Sun

Long

2013

Phys. Rev. C

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Within the relativistic Hartree-Fock-Bogoliubov (RHFB) theory, the structure properties of Carbon isotopes are systematically studied. To provide better overall description, the finite-range Gogny force D1S with an adjusted strength factor is adopted as the effective paring interaction in particle-particle channel. The selfconsistent RHFB calculations with density-dependent meson-nucleon couplings indicate the single-neutron halo structures in both 17 C and 19 C, whereas the two-neutron halo in 22 C is not well supported. It is also found that close to the neutron drip line there exists distinct odd-even staggering on neutron radii, which is tightly related with the blocking effects and correspondingly the blocking effect plays a significant role in the single-neutron halo formation.

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“…It is argued that they would be produced by including degrees of freedom beyond nucleons, e.g., hyperons, mesons, and quarks, or possibly produced by a better description of nucleonic interactions [11]. As a possible solution without exotic degrees of freedom, the relativistic mean-field (RMF) models is recalibrated with a soft behavior of the symmetry energy around saturation density [13,14].Compared to other CDF models, significant improvements have been obtained with DDRHF theory [10,15] in describing the relativistic symmetry conservation [15][16][17], the consistency of the isospin dependence in nuclear arXiv:1109.5428v2 [nucl-th] …”

mentioning

confidence: 99%

“…Compared to other CDF models, significant improvements have been obtained with DDRHF theory [10,15] in describing the relativistic symmetry conservation [15][16][17], the consistency of the isospin dependence in nuclear arXiv:1109.5428v2 [nucl-th]…”

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Hyperon effects in covariant density functional theory and recent astrophysical observations

et al. 2012

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Motivated by recent observational data, the equations of state with the inclusion of strangenessbearing Λ-hyperons and the corresponding properties of neutron stars are studied, based on the covariant density functional (CDF) theory. To this end, we specifically employ the density dependent relativistic Hartree-Fock (DDRHF) theory and the relativistic mean field theory (RMF). The inclusion of Λ-hyperons in neutron stars shows substantial effects in softening the equation of state. Because of the extra suppression effect originated from the Fock channel, large reductions on both the star mass and radius are predicted by the DDRHF calculations. It is also found that the mass-radius relations of neutron stars with Λ-hyperons determined by DDRHF with the PKA1 parameter set are in fairly good agreement with the observational data where a relatively small neutron stars radius is required. Therefore, it is expected that the exotic degrees of freedom such as the strangeness-bearing structure may appear and play significant roles inside the neutron stars, which is supported further by the systematical investigations on the consistency between the maximum neutron star mass and Λ-coupling strength. As the natural laboratories in the universe for nuclear and particle physics, neutron stars [1] have fascinated much effort concentrated on exploring the equation of state (EoS) of baryonic matter at low temperature and high density [2,3]. Specifically the mass of the observed neutron stars brings a strong constraint on the behavior of EoS at supranuclear density. The most precise measurements for the neutron star mass are determined to be less than 1.5M from the timing observations of radio binary pulsars [4], which has remained for many years to constraint the EoS. However, the existence of more massive compact stars is now unveiled by some evidence [5]. In a survey with the Arecibo telescope, an eccentric binary millisecond pulsar PSR J1903+0327 was found with an unusually high mass value (1.74 ± 0.04)M [6]. Recently a much larger pulsar mass of (1.97 ± 0.04)M was measured using Shapiro delay for the binary millisecond pulsar J1614-2230 [7]. All of these new data imply a stiff EoS of strongly interacting matter at high densities, which need further check on the new developed land-and space-based observatories.So far, there still exists considerable theoretical uncertainty on the EoS at supranuclear densities due to the poorly constrained many-body interaction, consequently deducing very different maximum mass and radius for a beta-stable neutron star. As indicated by prior study of neutron star based on the density dependent relativistic Hartree-Fock (DDRHF) theory [8], the maximum mass predicted by the covariant density functional (CDF) cal- * Electronic address: longwh@lzu.edu.cn culations [9,10] lies between 2M and 2.8M . The Corresponding EoSs deviate remarkably from each other at high density region. In the center of neutron stars, the density is generally considered as high as 5 to 10 times the nuclear equilibrium (satu...

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Pseudo-spin symmetry in density-dependent relativistic Hartree–Fock theory

Cited by 79 publications

References 29 publications

Recent progress and new challenges in isospin physics with heavy-ion reactions

Recent progress and new challenges in isospin physics with heavy-ion reactions

Description of carbon isotopes within relativistic Hartree-Fock-Bogoliubov theory

Hyperon effects in covariant density functional theory and recent astrophysical observations

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