Effects of ω meson self-coupling on the properties of finite nuclei and neutron stars

Kumar, Raj; Agrawal, B. K.; Dhiman, Shashi K.

doi:10.1103/physrevc.74.034323

Cited by 48 publications

(38 citation statements)

References 37 publications

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“…This is an alternative to the often-used method of constraining K 0 directly from its correlation with E GMR . Following this new approach, and by using experimental data of E GMR for 208 Pb, [112][113][114][115][116][117][118][119][120][121][122][123][124] Sn isotopes, 90 Zr, and 144 Sm, the linear correlation of E GMR and M c shown in Refs. [11,12] was used to constrain M c to the range M c = 1100 ± 70 MeV.…”

Section: B Updated Constraints: Set2a and Set2bmentioning

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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Section: B Updated Constraints: Set2a and Set2bmentioning

confidence: 99%

Relativistic mean-field hadronic models under nuclear matter constraints

et al. 2014

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“…The equations of state for these groups, e.g., the energy density and pressure, are calculated from the energy-momentum tensor (in the mean-field approximation): E = T 00 , and P = The results obtained were the following: out of 147 models only 9 of them satisfies all the constraints, excluding the constraint related to K τ,v (isospin dependence of the incompressibility) [1]. These are: BSR15, BSR16, BSR17 (5% of tolerance in the PNM2 constraint -see [1]), BSR18 (5% of tolerance in the PNM2 constraint -see [1]) [2], DD-F, [5] FSUGold, [6] FSUGold4, [7] FSUGZ06, [8] and TW99 [3]. Their nuclear matter properties are given in Table 1.…”

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confidence: 99%

Relativistic mean-field models and nuclear matter constraints

Dutra¹,

Lourenço²,

Carlson³

et al. 2013

AIP Conference Proceedings

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Abstract. This work presents a preliminary study of 147 relativistic mean-field (RMF) hadronic models used in the literature, regarding their behavior in the nuclear matter regime. We analyze here different kinds of such models, namely: (i) linear models, (ii) nonlinear σ 3 + σ 4 models, (iii) σ 3 + σ 4 + ω 4 models, (iv) models containing mixing terms in the fields σ and ω, (v) density dependent models, and (vi) point-coupling ones. In the finite range models, the attractive (repulsive) interaction is described in the Lagrangian density by the σ (ω) field. The isospin dependence of the interaction is modeled by the ρ meson field. We submit these sets of RMF models to eleven macroscopic (experimental and empirical) constraints, used in a recent study in which 240 Skyrme parametrizations were analyzed. Such constraints cover a wide range of properties related to symmetric nuclear matter (SNM), pure neutron matter (PNM), and both SNM and PNM.Keywords: relativistic models, asymmetric nuclear matter, constraints PACS: 21.30.Fe, 21.65.Cd, 21.65.Ef Quantum Hadrodynamics (QHD) is an approach based on quantum field theory much used in the description of hadronic environments, such as nuclear and neutron matter. It is based on local Lagrangian densities whose free parameters are adjusted in order to reproduce basic nuclear matter bulk properties at zero temperature. In general, nuclear matter is well described by different versions of the relativistic mean-field (RMF) models constructed via the QHD approach.In order to select a set of RMF models which better describe nuclear matter properties, as well as the physics of pure neutron matter, we submit 147 relativistic parameterizations to 11 constraints, out of which 4 are related to symmetric nuclear matter, 2 to pure neutron matter, and 5 related to the symmetry energy that involve both symmetric and pure neutron matter. All these constraints were taken at the saturation point (ρ 0 ), except the constraints related with the band region. For more details about the constraints and the criteria used for approval see Ref. [1].The relativistic hadronic models [2, 3, 4] used here are described by the following Lagrangian densities:

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“…The results are also compared to the corresponding experimental data. It is found that none of the published E-RMF parameter sets [10][11][12]14] were simultaneously compatible with all the constraints mentioned; but by fine tuning some parameters of the E-RMF model, agreement with experimental data has been achieved.…”

Section: Introductionmentioning

confidence: 98%

“…After that, several parameter sets of the model were introduced [11,12]. The parameter sets of the E-RMF model provide a good description of many ground-state properties of medium to heavy nuclei [10][11][12][13]. Efforts to improve the model's weakness in the isovector sector have also been made [12,14].…”

Section: Introductionmentioning

confidence: 99%

“…The parameter sets of the E-RMF model provide a good description of many ground-state properties of medium to heavy nuclei [10][11][12][13]. Efforts to improve the model's weakness in the isovector sector have also been made [12,14]. The impact of each of the additional couplings in the E-RMF model on the properties of nuclear matter, nuclear surface, and finite nuclei has also been discussed in detail in Refs.…”

Section: Introductionmentioning

confidence: 99%

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Fine tuning in an effective field based relativistic mean field model, and properties of neutron-rich matter

Sulaksono

Kasmudin

2009

Phys. Rev. C

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Properties of symmetric nuclear matter and neutron-rich matter predicted by effective field based relativistic mean field parameter sets are compared to those presented in a recent analysis of nuclear giant monopole resonance and isospin diffusion data and a study of the neutron skin of finite nuclei, as well as some selected observational data of neutron stars. Motivated by the fact that none of the published parameter sets of this model is simultaneously consistent with all previously mentioned constraints, an improvement not only in the isovector sector but also in isoscalar sector of this model is proposed. The properties of symmetric nuclear matter and neutron-rich matter, as well as some basic properties of static neutron stars predicted by the proposed parameter set (G2 * * ), are discussed.

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Effects of ω meson self-coupling on the properties of finite nuclei and neutron stars

Cited by 48 publications

References 37 publications

Relativistic mean-field hadronic models under nuclear matter constraints

Relativistic mean-field hadronic models under nuclear matter constraints

Relativistic mean-field models and nuclear matter constraints

Fine tuning in an effective field based relativistic mean field model, and properties of neutron-rich matter

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