Systematics of the bimodal isoscalar giant dipole resonance

Uchida, M.; Sakaguchi, H.; Itoh, Makoto; Yosoi, M.; Kawabata, T.; Yasuda, Yusuke; Takeda, Hiroyuki; Murakami, T.; Terashima, S.; Kishi, S.; Garg, U.; Boutachkov, P.; Hedden, M.; Kharraja, B.; Koss, Michael; Nayak, B. K.; Zhu, S.; Fujiwara, M̄.; Fujimura, H.; Yoshida, H. P.; Hara, K.; Akimune, H.; Harakeh, Mohsen

doi:10.1103/physrevc.69.051301

Cited by 100 publications

(99 citation statements)

References 30 publications

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“…Although in principle GMR energies of neutron-rich nuclei probe the incompressibility coefficient of neutron-rich matter [50], in practice the neutron-proton asymmetry for these nuclei is simply too small to provide any meaningful constraint on the density dependence of the symmetry energy. This is the main reason behind the agreement between FSU and FSU2, even though they predict radically different values for the slope of the symmetry energy L (see Table IV [61] and RCNP [62][63][64][65][66]. Theoretical results were obtained by following the constrained RMF formalism developed in Ref.…”

Section: Giant Monopole Resonancesmentioning

confidence: 99%

Building relativistic mean field models for finite nuclei and neutron stars

2014

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Background: Theoretical approaches based on density functional theory provide the only tractable method to incorporate the wide range of densities and isospin asymmetries required to describe finite nuclei, infinite nuclear matter, and neutron stars.Purpose: A relativistic energy density functional (EDF) is developed to address the complexity of such diverse nuclear systems. Moreover, a statistical perspective is adopted to describe the information content of various physical observables.Methods: We implement the model optimization by minimizing a suitably constructed χ 2 objective function using various properties of finite nuclei and neutron stars. The minimization is then supplemented by a covariance analysis that includes both uncertainty estimates and correlation coefficients.Results: A new model, "FSUGold 2 ", is created that can well reproduce the ground-state properties of finite nuclei, their monopole response, and that accounts for the maximum neutron star mass observed up to date. In particular, the model predicts both a stiff symmetry energy and a soft equation of state for symmetric nuclear matter-suggesting a fairly large neutron-skin thickness in 208 Pb and a moderate value of the nuclear incompressibility. Conclusions:We conclude that without any meaningful constraint on the isovector sector, relativistic EDFs will continue to predict significantly large neutron skins. However, the calibration scheme adopted here is flexible enough to create models with different assumptions on various observables. Such a scheme-properly supplemented by a covariance analysis-provides a powerful tool to identify the critical measurements required to place meaningful constraints on theoretical models.

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Section: Giant Monopole Resonancesmentioning

confidence: 99%

Building relativistic mean field models for finite nuclei and neutron stars

2014

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“…Isoscalar giant monopole resonances (ISGMRs) and isoscalar giant dipole resonances (ISGDR) are extensively examined by the MDA for the inelastic α scattering [1][2][3][4][5][6][7][8][9][10]. The ISGMR and ISGDR strength distributions were successfully extracted from continuous excitation-energy spectra by the MDA.…”

Section: Introductionmentioning

confidence: 99%

“…The ISGMR and ISGDR strength distributions were successfully extracted from continuous excitation-energy spectra by the MDA. These analyses gave the nuclear incompressibility of the symmetric nuclear matter [3,6,8]. Recently, inelastic α scattering off unstable nuclei becomes feasible [11,12] because ISGMRs in unstable nuclei are of special interest in nuclear physics to examine the nuclear incompressibility of the asymmetric nuclear matter.…”

Section: Introductionmentioning

confidence: 99%

Systematic analysis of inelastic α scattering off self-conjugate A=4n nuclei

Adachi¹,

Kawabata

Minomo

et al. 2018

Phys. Rev. C

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We systematically measured the differential cross sections of inelastic α scattering off self-conjugate A = 4n nuclei at two incident energies E α = 130 MeV and 386 MeV at Research Center for Nuclear Physics, Osaka University. The measured cross sections were analyzed by the distorted-wave Born-approximation (DWBA) calculation using the single-folding potentials, which are obtained by folding macroscopic transition densities with the phenomenological αN interaction. The DWBA calculation with the density-dependent αN interaction systematically overestimates the cross sections for the ΔL = 0 transitions. However, the DWBA calculation using the density-independent αN interaction reasonably well describes all the transitions with ΔL = 0-4. We examined uncertainties in the present DWBA calculation stemming from the macroscopic transition densities, distorting potentials, phenomenological αN interaction, and coupled channel effects in 12 C. It was found that the DWBA calculation is not sensitive to details of the transition densities nor the distorting potentials, and the phenomenological density-independent αN interaction gives reasonable results. The coupled-channel effects are negligibly small for the 2 + 1 and 3 − 1 states in 12 C, but not for the 0 + 2 state. However, the DWBA calculation using the density-independent interaction at E α = 386 MeV is still reasonable even for the 0 + 2 state. We concluded that the macroscopic DWBA calculations using the density-independent interaction are reliably applicable to the analysis of inelastic α scattering at E α ∼ 100 MeV/u.

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“…Having computed various ground-state properties one is now in a position to compute the linear response of the mean-field ground state to a variety of probes. In the present case we are interested in computing the isoscalar monopole response as probed, for example, in α-scattering experiments [28,[45][46][47][48]. Although the MF+RPA calculations carried out here follow closely the formalism developed in much greater detail in Ref.…”

Section: Formalismmentioning

confidence: 99%

“…The first two terms (κ and λ) are responsible for a softening of the equation of state of symmetric nuclear matter at normal density that results in a significant reduction of the incompressibility coefficient relative to that of the original Walecka model [41,43,44]. Indeed, such a softening is demanded by the measured distribution of isoscalar monopole strength in medium to heavy nuclei [13,21,28,[45][46][47][48][49]. Further, ω-meson self-interactions, as described by the parameter ζ , serve to soften the equation of state of symmetric nuclear matter at high densities and at present can only be meaningfully constrained by the limiting masses of neutron stars [50].…”

Section: Formalismmentioning

confidence: 99%

Giant monopole energies from a constrained relativistic mean-field approach

2013

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Background: Average energies of nuclear collective modes may be efficiently and accurately computed using a nonrelativistic constrained approach without reliance on a random phase approximation (RPA). Purpose: To extend the constrained approach to the relativistic domain and to establish its impact on the calibration of energy density functionals. Methods: Relativistic RPA calculations of the giant monopole resonance (GMR) are compared against the predictions of the corresponding constrained approach using two accurately calibrated energy density functionals. Results: We find excellent agreement-at the 2% level or better-between the predictions of the relativistic RPA and the corresponding constrained approach for magic (or semimagic) nuclei ranging from 16 O to 208 Pb. Conclusions: An efficient and accurate method is proposed for incorporating nuclear collective excitations into the calibration of future energy density functionals.

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Systematics of the bimodal isoscalar giant dipole resonance

Cited by 100 publications

References 30 publications

Building relativistic mean field models for finite nuclei and neutron stars

Building relativistic mean field models for finite nuclei and neutron stars

Systematic analysis of inelastic α scattering off self-conjugate A=4n nuclei

Giant monopole energies from a constrained relativistic mean-field approach

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