Asymmetric nuclear matter in the relativistic mean-field approach with vector cross interaction

Bunta, J. Kotulic; Gmuca, Stefan

doi:10.1103/physrevc.68.054318

Cited by 44 publications

(69 citation statements)

References 27 publications

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“…The HA parameter set further includes the isovector-scalar meson field δ and fits successfully some results obtained from the more microscopic DBHF approach [107]. The parameter sets NLρδ and DDRH-corr also include the isovector-scalar meson field δ, while PC-F2, PC-F4, PC-LA, and FKVW include the isovector-scalar interaction vertices.…”

Section: Resultsmentioning

confidence: 99%

“…For different versions of the RMF model considered in the present work, we mainly consider parameter sets commonly and successfully used in nuclear structure studies. In particular, we select the parameter sets NL1 [102], NL2 [102], NL3 [103], NL-SH [104], TM1 [105], PK1 [106], FSU-Gold [76], HA [107], NLρ [100], NLρδ [100] for the nonlinear RMF model; TW99 [46], DD-ME1 [108], DD-ME2 [109], PKDD [106], DD [93], DD-F [110], and DDRH-corr [47] for the densitydependent RMF model; and PC-F1 [49], PC-F2 [49], PC-F3 [49], PC-F4 [49], PC-LA [49], and FKVW [53] for the point-coupling RMF model. There are totally 23 parameter sets, and most of them can describe reasonably well the binding energies and charge radii of a large number of nuclei in the periodic table except the parameter set HA, for which to our knowledge there are no calculations for finite nuclei.…”

Section: Resultsmentioning

confidence: 99%

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Isospin-dependent properties of asymmetric nuclear matter in relativistic mean field models

2007

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Using various relativistic mean-field models, including the nonlinear ones with meson field selfinteractions, those with density-dependent meson-nucleon couplings, and the point-coupling models without meson fields, we have studied the isospin-dependent bulk and single-particle properties of asymmetric nuclear matter. In particular, we have determined the density dependence of nuclear symmetry energy from these different relativistic mean-field models and compare the results with the constraints recently extracted from analyses of experimental data on isospin diffusion and isotopic scaling in intermediate-energy heavy ion collisions as well as from measured isotopic dependence of the giant monopole resonances in even-A Sn isotopes. Among the 23 parameter sets in the relativistic mean-filed model that are commonly used for nuclear structure studies, only a few are found to give symmetry energies that are consistent with the empirical constraints. We have also studied the nuclear symmetry potential and the isospin-splitting of the nucleon effective mass in isospin asymmetric nuclear matter. We find that both the momentum dependence of the nuclear symmetry potential at fixed baryon density and the isospin-splitting of the nucleon effective mass in neutron-rich nuclear matter depend not only on the nuclear interactions but also on the definition of the nucleon optical potential.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Isospin-dependent properties of asymmetric nuclear matter in relativistic mean field models

2007

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“…In Ref. [238], the nuclear scalar densities are calculated using the non-linear RMF model with a Lagrangian density that includes the nucleon field ψ, the isoscalar-scalar meson field σ, the isoscalar-vector meson field ω, the isovector-vector meson field ρ, and the isovector-scalar meson field δ with three typical parameter sets, namely, the very successful NL3 model [252], the Z271v model, which has been used to study the neutron skin of heavy nuclei and the properties of neutron stars [223], and the HA model which includes the isovector-scalar meson field δ and fits successfully some results calculated with the more microscopic DBHF approach [253]. Fig.…”

Section: Nuclear Scalar Densitiesmentioning

confidence: 99%

“…For different versions of the RMF model considered in the above, we mainly consider parameter sets commonly and successfully used in nuclear structure studies. In particular, we select the parameter sets NL1 [310], NL2 [310], NL3 [252], NL-SH [311], TM1 [148], PK1 [312], FSU-Gold [75], HA [253], NLρ [308], NLρδ [308] for the nonlinear RMF model; TW99 [170], DD-ME1 [313], DD-ME2 [314], PKDD [312], DD [183], DD-F [315], and DDRH-corr [171] for the density-dependent RMF model; and PC-F1 [173], PC-F2 [173], PC-F3 [173], PC-F4 [173], PC-LA [173], and FKVW [142] for the point-coupling RMF model. There are totally 23 parameter sets, and most of them can describe reasonably well the binding energies and charge radii of a large number of nuclei in the periodic table except the parameter set HA, for which to our knowledge there are no calculations for finite nuclei.…”

Section: Rmf Model Predictions On the Symmetry Energy Symmetry Potenmentioning

confidence: 99%

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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“…DBHF represents four different parameterizations, chosen to describe matter in the framework of Dirac-Brueckner-Hartree-Fock theory. In particular, we choose the parameterizations labeled HA, HB, LA, and MA in Kotulič Bunta & Gmuca (2003) used by Urbanec et al (2010) to describe the properties of static neutron stars. The EoS labeled APR has often been used.…”

Section: Radiusmentioning

confidence: 99%

Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model

Urbanec

Török

Šrámková

et al. 2010

A&A

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The high-frequency quasi-periodic oscillations (HF QPOs) that appear in the X-ray fluxes of low-mass X-ray binaries remain an unexplained phenomenon. Among other ideas, it has been suggested that a non-linear resonance between two oscillation modes in an accretion disc orbiting either a black hole or a neutron star plays a role in exciting the observed modulation. Several possible resonances have been discussed. A particular model assumes resonances in which the disc-oscillation modes have the eigenfrequencies equal to the radial and vertical epicyclic frequencies of geodesic orbital motion. This model has been discussed for black hole microquasar sources as well as for a group of neutron star sources. Assuming several neutron (strange) star equations of state and Hartle-Thorne geometry of rotating stars, we briefly compare the frequencies expected from the model to those observed. Our comparison implies that the inferred neutron star radius R NS is larger than the related radius of the marginally stable circular orbit r ms for nuclear matter equations of state and spin frequencies up to 800 Hz. For the same range of spin and a strange star (MIT) equation of state, the inferrred radius is R NS ∼ r ms . The "Paczyński modulation" mechanism considered within the model requires that R NS < r ms . However, we find this condition to be fulfilled only for the strange matter equation of state, masses below 1 M , and spin frequencies above 800 Hz. This result most likely falsifies the postulation of the neutron star 3:2 resonant eigenfrequencies being equal to the frequencies of geodesic radial and vertical epicyclic modes. We suggest that the 3:2 epicyclic modes could stay among the possible choices only if a fairly non-geodesic accretion flow is assumed, or if a different modulation mechanism operates.

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Asymmetric nuclear matter in the relativistic mean-field approach with vector cross interaction

Cited by 44 publications

References 27 publications

Isospin-dependent properties of asymmetric nuclear matter in relativistic mean field models

Isospin-dependent properties of asymmetric nuclear matter in relativistic mean field models

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

Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model

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