Deducing the nuclear-matter incompressibility coefficient from data on isoscalar compression modes

Shlomo, S.; Kolomietz, V. M.; Colò, G.

doi:10.1140/epja/i2006-10100-3

Cited by 318 publications

(266 citation statements)

References 62 publications

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“…The values of the saturation parameters are E 0 =−15.9±0.4 MeV, n 0 = 0.164±0.007 fm −3 (Drischler et al 2016b), and K 0 =240± 20 MeV (Shlomo et al 2006;Piekarewicz 2010) or K 0 =230± 40 MeV (Khan et al 2012). In general, K sym <0 for realistic relativistic mean-field (RMF) and Skyrme forces, i.e., those that have been fit to properties of laboratory nuclei.…”

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy

Tews¹,

Lattimer²,

Ohnishi³

et al. 2017

ApJ

281

211

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We propose the existence of a lower bound on the energy of pure neutron matter (PNM) on the basis of unitary-gas considerations. We discuss its justification from experimental studies of cold atoms as well as from theoretical studies of neutron matter. We demonstrate that this bound results in limits to the density-dependent symmetry energy, which is the difference between the energies of symmetric nuclear matter and PNM. In particular, this bound leads to a lower limit to the volume symmetry energy parameter S 0 . In addition, for assumed values of S 0 above this minimum, this bound implies both upper and lower limits to the symmetry energy slope parameter L, which describes the lowest-order density dependence of the symmetry energy. A lower bound on neutron-matter incompressibility is also obtained. These bounds are found to be consistent with both recent calculations of the energies of PNM and constraints from nuclear experiments. Our results are significant because several equations of state that are currently used in astrophysical simulations of supernovae and neutron star mergers, as well as in nuclear physics simulations of heavy-ion collisions, have symmetry energy parameters that violate these bounds. Furthermore, below the nuclear saturation density, the bound on neutron-matter energies leads to a lower limit to the density-dependent symmetry energy, which leads to upper limits to the nuclear surface symmetry parameter and the neutron-star crust-core boundary. We also obtain a lower limit to the neutron-skin thicknesses of neutronrich nuclei. Above the nuclear saturation density, the bound on neutron-matter energies also leads to an upper limit to the symmetry energy, with implications for neutron-star cooling via the direct Urca process.

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Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy

Tews¹,

Lattimer²,

Ohnishi³

et al. 2017

ApJ

281

211

View full text Add to dashboard Cite

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“…The microscopic mean-field based RPA provides a good description of collective states in nuclei [1,8]. It is common to calculate the RPA states |n> with the corresponding energies E n , and obtain the strength function S(E) = Σ n |<0|F|n>| 2 δ(E-E n ), for a certain single particle scattering operator F = Σ f(i), and then determine the energy…”

Section: Description Of Microscopic Calculationsmentioning

confidence: 99%

“…This property of the ISGMR and the variation of the incompressibility coefficient with neutron number can also be used to extract the asymmetry coefficient K sym in the EOS of asymmetric NM [5]. In the analysis of experimental data on E 0 it is common to employ two approaches: (i) Adopting a semiclassical model to relate E 0 to an incompressibility coefficient K A of the nucleus and carry out a Leptodermous (A -1/3 ) expansion of K A , similar to a mass formula, to parameterize K A into volume, surface, symmetry and Coulomb terms [6,7]; and (ii) Carrying out microscopic calculations of the strength function S(E) of the ISGMR, within a fully self consistent mean-field based random phase approximation (RPA), with specific interactions (see the review [8]) and comparing with the experimental data. The values of K NM and K sym , are then deduced from the interaction that best reproduced the experimental data.…”

Section: Introductionmentioning

confidence: 99%

Isoscalar giant resonances inCa48

et al. 2011

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The giant resonance region from 9.5 MeV < E x < 40 MeV in 48 Ca has been studied with inelastic scattering of 240 MeV α particles at small angles, including 0º. 95±11% of E0 energy weighted sum rule (EWSR), 10 16 83 + − % of E2 EWSR and 137±20% of E1 EWSR were located below E x = 40 MeV. A comparison of the experimental data with calculated results for the isoscalar giant monopole resonance, obtained within the mean-field based random phase approximation, is also given.

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“…The study of collective modes in nuclei has been the subject of extensive theoretical and experimental studies during several decades [1][2][3], since it contributes significantly to our understanding of bulk properties of nuclei, their non-equilibrium properties and properties of the nuclear force. Of particular interest is the equation of state (EOS), i.e.…”

Section: Introductionmentioning

confidence: 99%

Giant resonances in40Ca and48Ca

et al. 2013

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We present results of fully self-consistent Hartree-Fock based random phase approximation calculations of the strength functions S(E) and centroid energies E CEN of isoscalar (T = 0) and isovector (T = 1) giant resonances of multipolarities L = 0 -3 in 40 Ca and 48 Ca, using a wide range of commonly employed 18 Skyrme type nucleonnucleon effective interactions. We determined the sensitivities of E CEN and of the isotopic differences E CEN ( 48 Ca) -E CEN ( 40 Ca) to physical quantities, such as nuclear matter incompressibility coefficient, symmetry energy density and effective mass, associated with the Skyrme interactions and compare the results with the available experimental data.

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Deducing the nuclear-matter incompressibility coefficient from data on isoscalar compression modes

Cited by 318 publications

References 62 publications

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy

Isoscalar giant resonances inCa48

Giant resonances in40Ca and48Ca

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