The Giant Monopole Resonance in the Sn Isotopes: Why is Tin so “Fluffy”?

Garg, U.; Li, T.; Okumura, Satoru; Akimune, H.; Fujiwara, M̄.; Harakeh, Mohsen; Hashimoto, Hitoshi; Itoh, Masatoshi; Iwao, Yuma; Kawabata, T.; Kawase, K.; Liu, Yuxuan; Marks, R.; Murakami, T.; Nakanishi, K.; Nayak, B. K.; Rao, P. V. Madhusudhana; Sakaguchi, H.; Terashima, Yutaka; Uchida, M.; Yasuda, Yusuke; Yosoi, M.; Zenihiro, J.

doi:10.1016/j.nuclphysa.2007.01.046

Cited by 94 publications

(61 citation statements)

References 42 publications

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“…[50], these features seem to suggest that the K τ = (−550 ± 100) MeV obtained in refs. [18,19] may suffer from the same ambiguities already encountered in earlier attempts [61] to extract the K 0 and K sat,2 of infinite matter from finite-nuclei extrapolations. This problem remains as an open challenge, and both experimental and theoretical insights are needed in the future.…”

Section: Discussionmentioning

confidence: 96%

“…In particular, using the empirical constraints of While the estimated value of −477 MeV K sat,2 −241 MeV in the present work has a small overlap with the constraint of K τ = (−550 ± 100) MeV obtained in refs. [18,19] from recent measurements of the isotopic dependence of the GMR in even-A Sn isotopes, the magnitude of the constrained K τ is still significantly larger than that of −477 MeV K sat,2 −241 MeV. Recently, there are several works [49,50] on extracting the value of the K sat,2 parameter based on the idea initiated by Blaizot and collaborators that the values of both K 0 and K sat,2 should be extracted from the same consistent theoretical model that successfully reproduces the experimental GMR energies of a variety of nuclei.…”

Section: Discussionmentioning

confidence: 99%

“…Most recently, a much stringent constraint of K τ = (−550 ± 100) MeV has been obtained in refs. [18,19] from measurements of the isotopic dependence of the GMR in even-A Sn isotopes.…”

Section: Equation Of State Of Asymmetric Nuclear Mattermentioning

confidence: 99%

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A phenomenological equation of state for isospin asymmetric nuclear matter

Chen

2009

Sci. China Ser. G-Phys. Mech. Astron.

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A phenomenological momentum-independent (MID) model is constructed to describe the equation of state (EOS) for isospin asymmetric nuclear matter, especially the density dependence of the nuclear symmetry energy Esym(ρ). This model can reasonably describe the general properties of the EOS for symmetric nuclear matter and the symmetry energy predicted by both the sophisticated isospin and momentum dependent MDI model and the Skyrme-Hartree-Fock approach. We find that there exists a nicely linear correlation between Ksym and L as well as between J 0 /K 0 and K 0 , where L and Ksym represent, respectively, the slope and curvature parameters of the symmetry energy at the normal nuclear density ρ 0 , while K 0 and J 0 are, respectively, the incompressibility and the third-order derivative parameter of symmetric nuclear matter at ρ 0 . These correlations together with the empirical constraints on K 0 , L and Esym(ρ 0 ) lead to an estimation of −477 MeV K sat,2 −241 MeV for the second-order isospin asymmetry expansion coefficient for the incompressibility of asymmetric nuclear matter at the saturation point. equation of state of nuclear matter, isospin, the symmetry energyThe study of the isospin degree of freedom in nuclear physics has recently attracted much attention due to the establishment of many radioactive beam facilities around the world. Besides the many existing radioactive beam facilities and their upgrades, such as the Cooling Storage Ring (CSR) facility at HIRFL in China [1] , many more are being constructed or under planning, including the Radioactive Ion Beam (RIB) Factory at RIKEN in Japan [2] , the FAIR/GSI in Germany [3] , SPIRAL2/GANIL in France [4] , and the Facility for Rare Isotope Beams (FRIB) in the USA [5] . These new facilities offer the possibility to study the properties of nuclear matter or nuclei under the extreme condition of large isospin asymmetry. The ultimate goal of such study is to extract information on the isospin dependence of in-medium nuclear effective interactions as well as the equation of state (EOS) of isospin asymmetric nuclear matter, particularly its isospin-dependent term or the density dependence of the nuclear symmetry energy. This knowledge, especially the latter, is important for understand-

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Section: Discussionmentioning

confidence: 96%

Section: Discussionmentioning

confidence: 99%

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A phenomenological equation of state for isospin asymmetric nuclear matter

Chen

2009

Sci. China Ser. G-Phys. Mech. Astron.

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“…The properties of asymmetric nuclear systems have also been studied in terrestrial laboratories in past years [2,3], but many aspects still rely on theoretical models. Constraints on the behavior of the symmetry energy above nuclear saturation density have been coming from experiments with new neutron-rich radioactive beams, and in relativistic heavy-ion collisions, giant monopole resonances [4], isobaric analog states [5], or meson production (pions [6] and kaons [7]) in heavy-ion collisions.…”

Section: Introductionmentioning

confidence: 99%

Correlation of the neutron star crust-core properties with the slope of the symmetry energy and the lead skin thickness

et al. 2016

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The correlations of the crust-core transition density and pressure in neutron stars with the slope of the symmetry energy and the neutron skin thickness are investigated, using different families of relativistic mean-field parametrizations with constant couplings and nonlinear terms mixing the σ -, ω-, and ρ-meson fields. It is shown that the modification of the density dependence of the symmetry energy, involving the σ or the ω meson, gives rise to different behaviors: the effect of the ω meson may also be reproduced within nonrelativistic phenomenological models, while the effect of the σ meson is essentially relativistic. Depending on the parametrization with σ -ρ or ω-ρ mixing terms, different values of the slope of the symmetry energy at saturation must be considered in order to obtain a neutron matter equation of state compatible with results from chiral effective field theory. This difference leads to different pressures at the crust-core transition density. A linear correlation between the transition density and the symmetry energy slope or the neutron skin thickness of the 208 Pb nucleus is obtained, only when the ω meson is used to describe the density dependence of the symmetry energy. A comparison is made between the crust-core transition properties of neutron stars obtained by three different methods, the relativistic random phase approximation (RRPA), the Vlasov equation, and thermodynamical method. It is shown that the RRPA and the Vlasov methods predict similar transition densities for pne β-equilibrium stellar matter.

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“…The nEoS governs many aspects of astrophysics such as neutron star physics and nucleosynthesis during the explosive death of stars [4][5][6][7]. In terrestrial environments, the nEoS is integral in explaining the neutron skin thickness of heavy nuclei, collective excitations of nuclei, and the dynamics of heavy-ion collisions [8][9][10].…”

mentioning

confidence: 99%