Constraints on Skyrme equations of state from doubly magic nuclei, 
<i>ab initio</i>
 calculations of low-density neutron matter, and neutron stars

Tsang, C. Y.; Brown, B. A.; Fattoyev, F. J.; Lynch, W. G.; Tsang, M. B.

doi:10.1103/physrevc.100.062801

Cited by 16 publications

(7 citation statements)

References 69 publications

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“…The surviving sets tentatively suggest the following ranges of parameters, (J, L) CS+NS+OS ≈ (30 − 32, 45 − 65) MeV. (14) slightly extending the range suggested in Eq. (13).…”

Section: B Neutron Star Mass-radius Relation and Tidal Deformabilitysupporting

confidence: 67%

“…Another important feature of the KIDS framework is that assumptions for the EoS parameters are independent of assumptions for the in-medium effective mass. The effective mass is decoupled from the EoS of homogeneous matter and cannot contaminate our constraints on the latter -as could be the case in more restricted ansaetze [14,15], see also Sec. II C.…”

Section: A Kids Frameworkmentioning

confidence: 95%

“…or roughly 42 −3(µ −1 v − 1) + 4(µ −1 s − 1) MeV fm 2 /ρ 0 . In addition, given the strong contribution of the kinetic terms (a 2 , b 2 ) to the density dependence, strong limitations must be considered for the effective mass to better control the EoS parameters and the neutron-star massradius relation [14].…”

Section: Underdetermined Eos's?mentioning

confidence: 99%

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Constraining the density dependence of the symmetry energy with nuclear data and astronomical observations in the Korea-IBS-Daegu-SKKU framework

et al. 2021

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Background: The properties of very neutron rich nuclear systems are largely determined by the density dependence of the nuclear symmetry energy. The KIDS framework for the nuclear equation of state (EoS) and energy density functional (EDF) offers the possibility to explore the symmetryenergy parameters such as J (value at saturation density), L (slope at saturation), Ksym (curvature at saturation) and higher-order ones independently of each other and independently of assumptions about the in-medium effective mass, as previously shown in the cases of closed-shell nuclei and neutron-star properties. Purpose: We examine the performance of EoSs with different symmetry energy parameters on properties of nuclei and observations of neutron stars and gravitational waves in an effort to constrain in particular L and Ksym or the droplet-model counterpart Kτ . Method: Assuming a standard EoS for symmetric nuclear matter, we explore several points on the hyperplane of (J, L, Ksym or Kτ ) values. For each point, the corresponding KIDS functional parameters and a pairing parameter are obtained for applications in spherical even-even nuclei. This is the first application of KIDS energy density functionals with pairing correlations in a spherical HFB computational code. The different EoSs are tested successively on the properties of closed-shell nuclei, along the Sn isotopic chain, and on astronomical observations, in a step-by-step procedure of elimination and correction. Results: A small regime of best-performing parameters is determined and correlations between symmetry-energy parameters are critically discussed. The results strongly suggest that Ksym is negative and no lower than −200 MeV, that Kτ lies between roughly −400 and −300 MeV and that L lies between 40 and 65 MeV, with L 55MeV more likely. For the selected well-performing sets, corresponding predictions for the position of the neutron drip line and the neutron skin thickness of selected nuclei are reported. The results are only weakly affected by the choice of effective mass values. Parts of the drip line can be sensitive to the symmetry energy parameters. Conclusion: Using KIDS EoSs for unpolarized homogeneous matter at zero temperature and KIDS EDFs with pairing correlations in spherical symmetry we have explored the hyperplane of symmetryenergy parameters. Using both nuclear-structure data and astronomical observations as a testing ground, a narrow regime of well-performing parameters has been determined, free of non-physical correlations and decoupled from constraints on the nucleon effective mass. The results underscore the role of Kτ and of precise astronomical observations. More-precise constraints are possible with precise fits to nuclear energies and, in the future, more-precise input from astronomical observations.

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“…The surviving sets tentatively suggest the following ranges of parameters, (J, L) CS+NS+OS ≈ (30 − 32, 45 − 65) MeV. (14) slightly extending the range suggested in Eq. (13).…”

Section: B Neutron Star Mass-radius Relation and Tidal Deformabilitysupporting

confidence: 67%

Section: A Kids Frameworkmentioning

confidence: 95%

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Constraining the density dependence of the symmetry energy with nuclear data and astronomical observations in the Korea-IBS-Daegu-SKKU framework

et al. 2021

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“…The brown ellipse is the bound obtained from SkΛ267 model within the 1σ confidence. This bound has good overlap with the recent result obtained with APR2 [59] and ELYO −s+p [58] and agrees marginally with the ones obtained by Most et al [14] and Tsang et al [57]. It may be pointed out that the results for Most et al is within 2σ limits and obtained without considering bounds from microscopic finite nuclei experiments.…”

supporting

confidence: 88%

Unveiling the correlations of tidal deformability with the nuclear symmetry energy parameters

Malik,

Agrawal,

Providência

et al. 2020

Preprint

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The chi-squared based covariance approach allows one to estimate the correlations among desired observables related to nuclear matter directly from a set of fit data without taking recourse to the distributions of the nuclear matter parameters (NMPs). Such an approach is applied to study the correlations of tidal deformability of neutron star with the slope and the curvature parameters of nuclear symmetry energy governed by an extensive set of fit data on the finite nuclei together with the maximum mass of the neutron star. The knowledge of the distributions of NMPs consistent with the fit data is implicitly inbuilt in the Hessian matrix which is central to this covariance approach. Comparing our results with those obtained with the explicit use of the distributions of NMPs, we show that the appropriate correlations among NMPs as induced by the fit data are instrumental in strengthening the correlations of the tidal deformability with the symmetry energy parameters, without it, the said correlations tend to disappear. The interplay between isoscalar and isovector NMPs is also emphasized.

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“…nuclei close to the stability valley [16]. Novel strategies to constrain the EDF on microscopic calculations of PNM have been developed [16][17][18][19][20][21] to accompany the growing experimental research efforts devoted to unstable nuclei at the limits of the nuclear chart. Their success however, relies on accurate microscopic calculations of the EOS, supplemented by reliable estimates of theoretical uncertainties.…”

Section: Introductionmentioning

confidence: 99%

Benchmark calculations of infinite neutron matter with realistic two- and three-nucleon potentials

Lovato,

Bombaci,

Logoteta

et al. 2022

Preprint

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Constraints on Skyrme equations of state from doubly magic nuclei, ab initio calculations of low-density neutron matter, and neutron stars

Cited by 16 publications

References 69 publications

Constraining the density dependence of the symmetry energy with nuclear data and astronomical observations in the Korea-IBS-Daegu-SKKU framework

Constraining the density dependence of the symmetry energy with nuclear data and astronomical observations in the Korea-IBS-Daegu-SKKU framework

Unveiling the correlations of tidal deformability with the nuclear symmetry energy parameters

Benchmark calculations of infinite neutron matter with realistic two- and three-nucleon potentials

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