Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Lim, Yeunhwan; Holt, Jeremy W.

doi:10.1140/epja/i2019-12917-9

Cited by 86 publications

(65 citation statements)

References 140 publications

(190 reference statements)

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“…9. This clearly shows that varying R sym affects the nuclear symmetry energy only at densities larger than 0.6 ∼ 0.7 fm −3 which is within the range of maximum central density of neutron stars [20]. Since R5a, R5b, and R5c give similar symmetry energy below this density, they would give similar results for neutron stars.…”

Section: Expansion In Asymmetric Partmentioning

confidence: 54%

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Analysis of nuclear structure in a converging power expansion scheme

et al. 2019

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Background: In the framework of the newly developed generalized energy density functional (EDF) called KIDS, the nuclear equation of state (EoS) is expressed as an expansion in powers of the Fermi momentum or the cubic root of the density (ρ 1/3 ). Although an optimal number of converging terms was obtained in specific cases of fits to empirical data and pseudodata, the degree of convergence remains to be examined not only for homogeneous matter but also for finite nuclei. Furthermore, even for homogeneous matter, the convergence should be investigated with widely adopted various EoS properties at saturation.Purpose: The first goal is to validate the minimal and optimal number of EoS parameters required for the description of homogeneous nuclear matter over a wide range of densities relevant for astrophysical applications. The major goal is to examine the validity of the adopted expansion scheme for an accurate description of finite nuclei.Method: We vary the values of the high-order density derivatives of the nuclear EoS, such as the skewness of the energy of symmetric nuclear matter and the kurtosis of the symmetry energy, at saturation and examine the relative importance of each term in ρ 1/3 expansion for homogeneous matter. For given sets of EoS parameters determined in this way, we define equivalent Skyrme-type functionals and examine the convergence in the description of finite nuclei focusing on the masses and charge radii of closed-shell nuclei.Results: The EoS of symmetric nuclear matter is found to be efficiently parameterized with only 3 parameters and the symmetry energy (or the energy of pure neutron matter) with 4 parameters when the EoS is expanded in the power series of the Fermi momentum. Higher-order EoS parameters do not produce any improvement, in practice, in the description of nuclear ground-state energies and charge radii, which means that they cannot be constrained by bulk properties of nuclei.Conclusions: The minimal nuclear EDF obtained in the present work is found to reasonably describe the properties of closed-shell nuclei and the mass-radius relation of neutron stars. Attempts at refining the nuclear EDF beyond the minimal formula must focus on parameters which are not active (or strongly active) in unpolarized homogeneous matter, for example, effective tensor terms and time-odd terms. * Electronic address: gil@knu.ac.kr † Electronic address: ymkim715@gmail.com ‡ Electronic address: hch@daegu.ac.kr § Electronic address: ppapakon@ibs.re.kr ¶ Electronic address: yohphy@knu.ac.kr the fits, a robust parameter set was chosen as a baseline for further explorations, comprising three terms for isospin-symmetric nuclear matter (SNM) and four for pure neutron matter (PNM). The naturalness of the expansion was confirmed and extrapolations to extreme density regimes, were found to be satisfactory [4]. In particular, the extrapolated results agreed with ab initio calculations for dilute neutron matter, a regime to which the model had not been fitted at all, and reproduced a realistic mass-radius ...

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Section: Expansion In Asymmetric Partmentioning

confidence: 54%

“…[1]. Fitted values of parameters and the corresponding χ 2 n defined as [1] 20) are shown in Table IV. They are referred to as model PN for N = (3,4,5,6).…”

Section: Expansion In Asymmetric Partmentioning

confidence: 99%

Analysis of nuclear structure in a converging power expansion scheme

et al. 2019

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“…5 [86]. Furthermore, many theoretical works also presented their constraints on the density dependence of symmetry energy, like the chiral effective theory [87,88]. Therefore, in…”

Section: The Relativistic Brueckner-hartree-fock Model In Nu-cleamentioning

confidence: 99%

Properties of nuclear matter in relativistic Brueckner–Hartree–Fock model with high-precision charge-dependent potentials

Wang

Zhang

et al. 2020

J. Phys. G: Nucl. Part. Phys.

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Properties of nuclear matter are investigated in the framework of relativistic Brueckner-Hartree-Fock model with the latest high-precision charge-dependent Bonn (pvCD-Bonn) potentials, where the coupling between pion and nucleon is adopted as pseudovector form. These realistic pvCD-Bonn potentials are renormalized to effective nucleon-nucleon (N N) interactions, G matrices. They are obtained by solving the Blankenbecler-Sugar (BbS) equation in nuclear medium. Then, the saturation properties of symmetric nuclear matter are calculated with pvCD-Bonn A, B, C potentials. The energies per nucleon are around −10.72 MeV to −16.83 MeV at saturation densities, 0.139 fm −3 to 0.192 fm −3 with these three potentials, respectively. It clearly demonstrates that the pseudovector coupling between pion and nucleon can generate reasonable saturation properties comparing with pseudoscalar coupling. Furthermore, these saturation properties have strong correlations with the tensor components of N N potentials, i.e., the D-state probabilities of deuteron, P D to form a relativistic Coester band. The equations of state of pure neutron matter from pvCD-Bonn potentials are almost identical, since the prominent difference of pvCD Bonn potentials are the components of tensor force, which provides very weak contributions in the case of total isospin T = 1. In addition, the charge symmetry breaking (CSB) and charge independence breaking (CIB) effects are also discussed in nuclear matter from the partial wave contributions with these highprecision charge-dependent potentials. In general, the magnitudes of CSB from the differences between nn and pp potentials are about 0.05 MeV, while those of CIB are around 0.35 MeV from the differences between np and pp potentials. Finally, the equations of state of asymmetric nuclear matter are also calculated with different asymmetry parameters. It is found that the effective neutron mass is larger than the proton one in neutron-rich matter.

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“…There are also many studies reported the maximum mass of NSs from analyzing data extracted from gravitational wave (GW) events (see the recent review in Refs. [6,7], and the references therein). Note that Lim and Holt [7] discussed the Bayesian modeling of the nuclear equation of state (EOS) systematically, assuming a minimal model at high-density and neglect the possibility of phase transition for NS tidal deformability and GW170817 by generating 300000 NS EOSs by sampling from Bayesian posterior probability distributions.…”

Section: Introductionmentioning

confidence: 99%

“…[6,7], and the references therein). Note that Lim and Holt [7] discussed the Bayesian modeling of the nuclear equation of state (EOS) systematically, assuming a minimal model at high-density and neglect the possibility of phase transition for NS tidal deformability and GW170817 by generating 300000 NS EOSs by sampling from Bayesian posterior probability distributions. The obtained tidal deformability and the radius range of the canonical NS are consistent with observational constraints from GW170817, but 30% of the EOS fail to generate 2.0 M maximum mass constraint.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic neutron stars with hyperons: implication of the recent nuclear matter data and observations of neutron stars

et al. 2020

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Motivated by a recent report by Biwas and Bose (Phys Rev D 99:104002, 2019) that the observations of GW170817 to constrain the extent of pressure anisotropy in neutron stars within Bower–Liang anisotropic model, we systematically study the effects of anisotropic pressure on properties of the neutron stars with hyperons. The equation of state is calculated using the relativistic mean-field model with a BSP parameter set to determine nucleonic coupling constants and by using SU(6) and hyperon potential depths to determine hyperonic coupling constants. We investigate three models of anisotropic pressure known in literature namely Bowers and Liang (Astrophys J 88:657, 1974), Horvat et al. (Class Quant Grav 28:025009, 2011), and Cosenza et al. (J Math Phys (NY) 22:118, 1981). The reliability of the equation of state used is checked by comparing the parameters of the corresponding EOS to recent experimental data. The mass–radius, moment of inertia, and tidal deformability results of Bowers–Liang, Horvat et al., and Cosenza et al. anisotropic models are compared to the corresponding recent results extracted from the analysis of some NS observation data. We have found that the radii predicted by anisotropic NS are sensitive to the anisotropic model used and the results obtained by using the model proposed by Horvat et al. with anisotropic free parameter $$\varUpsilon ~\approx -$$Υ≈- 1.15 are relative compatible with all taken constraints.

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Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Cited by 86 publications

References 140 publications

Analysis of nuclear structure in a converging power expansion scheme

Analysis of nuclear structure in a converging power expansion scheme

Properties of nuclear matter in relativistic Brueckner–Hartree–Fock model with high-precision charge-dependent potentials

Anisotropic neutron stars with hyperons: implication of the recent nuclear matter data and observations of neutron stars

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