Correlations between the nuclear matter symmetry energy, its slope, and curvature from a nonrelativistic solvable approach and beyond

Santos, Bruna Michalski dos; Dutra, M.; Lourenço, O.; Delfino, A.

doi:10.1103/physrevc.90.035203

Cited by 24 publications

(25 citation statements)

References 79 publications

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“…The slope parameter L = 3ρ∂S(ρ)/∂ρ| ρ 0 and curvature parameter K sym = 9ρ 2 ∂ 2 S/∂ρ 2 | ρ 0 characterize the density-dependent behavior of the symmetry energy around ρ 0 . Extensive independent studies have been performed to constrain the slope L, but the uncertainty is still large [15][16][17][18].…”

Section: Introductionmentioning

confidence: 99%

Constraints on neutron skin thickness inPb208and density-dependent symmetry energy

Dong

Zuo

2015

Phys. Rev. C

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Accurate knowledge about the neutron skin thickness ∆R np in 208 Pb has far-reaching implications for different communities of nuclear physics and astrophysics. Yet, the novel Lead Radius Experiment (PREX) did not yield stringent constraint on the ∆R np recently. We employ a more practicable strategy currently to probe the neutron skin thickness of 208 Pb based on a high linear correlation between the ∆R np and J −a sym , where J and a sym are the symmetry energy (coefficient) of nuclear matter at saturation density and of 208 Pb. An accurate J − a sym thus places a strong constraint on the ∆R np . Compared with the parity-violating asymmetry A PV in the PREX, the reliably experimental information on the J − a sym is much more easily available attributed to a wealth of measured data on nuclear masses and on decay energies. The density dependence of the symmetry energy is also well constrained with the J − a sym . Finally, with a 'tomoscan' method, we find that one just needs to measure the nucleon densities in 208 Pb starting from R m = 7.61 ± 0.04 fm to obtain the ∆R np in hadron scattering experiments, regardless of its interior profile that is hampered by the strong absorption.Here we adopt the union of the two values, i.e. J = 32.4 ± 0.6 MeV, and hence the central issue is to determine the symmetry energy a sym of 208 Pb accurately. We extract the mass dependent symmetry energy a sym (A) = J/(1 + κA 1/3 ) [40,41] with β − -decay energies Q β − of heavy odd-A nuclei and with mass differences ∆B between A (Z − 1) and A (Z + 1) as our previous calculations [42,43] but with a new input quantity J, and then derive the a sym of 208 Pb. The merit of these two approaches is that only the well known Coulomb energy survives in Q β − and in ∆B when determining the unknown a sym , where the Q β − and ∆B are all taken from experimental data. Consequently, the a sym is extracted to be 22.4 ± 0.4MeV accurately, which is quite insensitive to the input quantity J. As a result, the derived J − a sym is 10.0 ± 1.0 MeV (solid circle in Fig. 1), which allows us to constrain the neutron skin thickness as well as the slope L in our subsequent calculations.The neutron skin thickness in 208 Pb is predicted to be ∆R np = 0.176 ± 0.021 fm (solid square in Fig. 1), where the estimated error stems from the uncertainties of the J − a sym as well as Eq. (2). To reach such an error level, the A PV in the PREX should be measured at least up to 2% accuracy, which is hardly implemented at present. This fact indicates the J − a sym is much more effective to probe the ∆R np currently. The precise information about the ∆R np is of fundamental importance and has far-reaching implications in neutron star physics, such as the structure, composition and cooling. As an example, a relation of ρ c ≈ 0.16 − 0.39∆R np was put forward to describe the relation between the ∆R np of 208 Pb and the transition density ρ c from a solid neutron star crust to the liquid interior [44], where the ρ c is estimated to be 0.091 ± 0.008 fm −3 . The properties of the cru...

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Section: Introductionmentioning

confidence: 99%

Constraints on neutron skin thickness inPb208and density-dependent symmetry energy

Dong

Zuo

2015

Phys. Rev. C

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“…Once the incompressibility at saturation is fixed, the IVGDR 208 Pb may be used to constrain the symmetry energy. Although not conclusive, there seems to exist a correlation among the values of J , L 0 , and the curvature (K 0 sym ) of the symmetry energy at the saturation density [23][24][25], and we tackle this point later.…”

Section: Introductionmentioning

confidence: 99%

Relativistic mean-field hadronic models under nuclear matter constraints

et al. 2014

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Background:The microscopic composition and properties of infinite hadronic matter at a wide range of densities and temperatures have been subjects of intense investigation for decades. The equation of state (EoS) relating pressure, energy density, and temperature at a given particle number density is essential for modeling compact astrophysical objects such as neutron stars, core-collapse supernovae, and related phenomena, including the creation of chemical elements in the universe. The EoS depends not only on the particles present in the matter, but, more importantly, also on the forces acting among them. Because a realistic and quantitative description of infinite hadronic matter and nuclei from first principles in not available at present, a large variety of phenomenological models has been developed in the past several decades, but the scarcity of experimental and observational data does not allow a unique determination of the adjustable parameters. Purpose: It is essential for further development of the field to determine the most realistic parameter sets and to use them consistently. Recently, a set of constraints on properties of nuclear matter was formed and the performance of 240 nonrelativistic Skyrme parametrizations was assessed [M. Dutra et al., Phys. Rev. C 85, 035201 (2012)] in describing nuclear matter up to about three times nuclear saturation density. In the present work we examine 263 relativistic-mean-field (RMF) models in a comparable approach. These models have been widely used because of several important aspects not always present in nonrelativistic models, such as intrinsic Lorentz covariance, automatic inclusion of spin, appropriate saturation mechanism for nuclear matter, causality, and, therefore, no problems related to superluminal speed of sound in medium. Method: Three different sets of constraints related to symmetric nuclear matter, pure neutron matter, symmetry energy, and its derivatives were used. The first set (SET1) was the same as used in assessing the Skyrme parametrizations. The second and third sets (SET2a and SET2b) were more suitable for analysis of RMF and included, up-to-date theoretical, experimental and empirical information. Results: The sets of updated constraints (SET2a and SET2b) differed somewhat in the level of restriction but still yielded only 4 and 3 approved RMF models, respectively. A similarly small number of approved Skyrme parametrizations were found in the previous study with Skyrme models. An interesting feature of our analysis 0556-2813/2014/90(5)/055203 (35) 055203-1 ©2014 American Physical Society M. DUTRA et al.PHYSICAL REVIEW C 90, 055203 (2014) has been that the results change dramatically if the constraint on the volume part of the isospin incompressibility (K τ,v ) is eliminated. In this case, we have 35 approved models in SET2a and 30 in SET2b. Conclusions: Our work provides a new insight into application of RMF models to properties of nuclear matter and brings into focus their problematic proliferation. The assessment performed in this wo...

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“…Stronger correlations are found among the isovector parameters, which are corr(E sym , L sym ) = 0.67 and corr(L sym , K sym ) = 0.67. The former is found in several works (see References [23,26,65] and references therein for a review), and the latter is also studied in References [66][67][68][69][70][71][72]. Slight correlations between high-order parameters, K sat − Q sat and K sym − Q sym , are also induced due to the narrow EFT energy bands at very low densities.…”

Section: Pearson Correlationsmentioning

confidence: 85%

The Nuclear Matter Density Functional under the Nucleonic Hypothesis

2021

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A Bayesian analysis of the possible behaviors of the dense matter equation of state informed by recent LIGO-Virgo as well as NICER measurements reveals that all the present observations are compatible with a fully nucleonic hypothesis for the composition of dense matter, even in the core of the most massive pulsar PSR J0740+6620. Under the hypothesis of a nucleonic composition, we extract the most general behavior of the energy per particle of symmetric matter and density dependence of the symmetry energy, compatible with the astrophysical observations as well as our present knowledge of low-energy nuclear physics from effective field theory predictions and experimental nuclear mass data. These results can be used as a null hypothesis to be confronted with future constraints on dense matter to search for possible exotic degrees of freedom.

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Correlations between the nuclear matter symmetry energy, its slope, and curvature from a nonrelativistic solvable approach and beyond

Cited by 24 publications

References 79 publications

Constraints on neutron skin thickness inPb208and density-dependent symmetry energy

Constraints on neutron skin thickness inPb208and density-dependent symmetry energy

Relativistic mean-field hadronic models under nuclear matter constraints

The Nuclear Matter Density Functional under the Nucleonic Hypothesis

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