Tensor and Coulomb-exchange terms in the relativistic mean-field model with 
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-meson and isoscalar-isovector coupling

Liliani, Netta; Diningrum, Jenny Primanita; Sulaksono, A.

doi:10.1103/physrevc.104.015804

Cited by 5 publications

(11 citation statements)

References 108 publications

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“…the constraints that we adopted in this work i.e., From the table above, all values in the parameter sets will decrease with increased the 2   value, except for the incompressibility K. At first glance we think, the value in PTE16 can be minimized until reaches the maximum constraint, but in our previous work [5], slope L from PTE15 has reached 77.574 MeV. So, PTE16 and PTE31 have reached the maximum and minimum values of the constraints above.…”

Section: Nuclear Matter Propertiesmentioning

confidence: 90%

“…In this section we briefly review the formalism of the RMF model with additional tensor couplings, the coulomb exchange and the various isovector-isoscalar couplings, with the equations and the step of fitting in Ref. [5,11]. The Lagrangian density of the RMF model is:…”

Section: Methodsmentioning

confidence: 99%

“…The value of each parameter set was obtained by a fitting process with the experimental data of finite nuclei observables [3], using a similar fitting protocol used in Refs. [5,11]. Here, we used the experimental data of the 14 nuclei binding energies and 13 nuclei charge radius of, and also used parameterization weight in order of 0.15% and 0.3% for the binding energies and charge radius, respectively.…”

Section: Parametrizationmentioning

confidence: 99%

“…The other fundamental physical observable is neutron skin thickness np r  , is defined by the difference between the neutron and proton root-mean-square radius, are indispensable in nuclear reaction and nuclear astrophysics research [5]. Motivated by the finding of the author's previous work [5,11] that the tensor couplings, Coulomb exchange EM EXC C and isovector-isoscalar coupling 2   terms in the RMF model have an impact on the neutron skin thickness of nuclei prediction, a peculiarity of significantly thick skin thickness of 208 Pb [12]. In this work, we will investigate the minimum and maximum values of isovector-isoscalar coupling that are compatible with the constraints in Ref.…”

Section: Introductionmentioning

confidence: 99%

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Role of Isovector-Isoscalar Coupling on Charge Radius of Heavy and Superheavy Nuclei

Liliani

2022

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We have investigated the effect of the isovector-isoscalar coupling on the finite nuclei and nuclear matter properties, the neutron skin thickness of 208Pb, and the charge radius on heavy and superheavy nuclei calculated by the relativistic mean-field (RMF) model. In this work, we generates two parameter sets, i.e., PTE16 and PTE31. The numbers 16 and 31 denote the isovector-isoscalar coupling terms, while T and E denote the tensor coupling and electromagnetic exchange terms, respectively. We found that PTE16 and PTE31 are compatible with the constraints obtained by R. Essick, et al., arXiv: 2102.10074v1 [nucl-th] (2021). We also found that the increase of the isovector-isoscalar coupling terms gives a significant effect on the binding energy and the charge radius on heavy nuclei except for the charge radius of 208Pb. Increased of the isovector-isoscalar coupling terms make the values of charge radius prediction increase too, but vice versa for the neutron skin thickness and nuclear matter prediction. PTE31 yields symmetry energy J = 31.521 MeV, slope L = 57.643 MeV, and neutron skin thickness = 0.21419 fm. While the β2 correction (for deform nuclei) does not always give a significant effect on the charge radius.

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Section: Nuclear Matter Propertiesmentioning

confidence: 90%

Section: Methodsmentioning

confidence: 99%

Section: Parametrizationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Role of Isovector-Isoscalar Coupling on Charge Radius of Heavy and Superheavy Nuclei

Liliani

2022

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“…For detailed discussions related to SNM and PNM predicted by standard RMF models and their compatibility with exper-imental data and NS properties predictions, please see Ref. [32][33][34][35][36] and the references therein. In this work, we will also show that when we consider GUP correction in the EoS of matter, the first law of thermodynamics is preserved only if the pressure of matter is anisotropic.…”

Section: Introductionmentioning

confidence: 99%

Minimal length, nuclear matter, and neutron stars

et al. 2022

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In this paper, we employ one variant of the Generalized Uncertainty Principle (GUP) model, i.e., the Kempf–Mangano–Mann (KMM) model, and discuss the impact of GUP on the EoS of nuclear and neutron star matter based on the relativistic mean field (RMF) model. We input the result in the Serrano–Liška (SL) gravity theory to discuss the corresponding Neutron Star (NS) properties. We have shown that the upper bound for the GUP parameter from nuclear matter properties is $$\beta \le 2\times 10^{-7}$$ β ≤ 2 × 10 - 7 MeV$$^{-2}$$ - 2 . If we used this $$\beta $$ β upper bound to calculate NS matter, and considering SL parameter $${\tilde{c}}$$ c ~ as an independent parameter, we have found that the upper bound for the SL parameter, which modifies the Einstein field equation, is $${\tilde{c}} \le 10^7$$ c ~ ≤ 10 7 m$$^2$$ 2 . This beta upper bound is determined by considering the anisotropy magnitude smaller than the pressure magnitude. By employing $$\beta =2\times 10^{-7}$$ β = 2 × 10 - 7 MeV$$^{-2}$$ - 2 and $${\tilde{c}} = 10^7$$ c ~ = 10 7 m$$^2$$ 2 , we obtain the mass–radius relation that satisfies NICER data for both PSR J0740+6620 (whose mass is $$\sim 2.1M_\odot $$ ∼ 2.1 M ⊙ ) and PSR J0030+0451 ($$M\sim 1.4M_\odot $$ M ∼ 1.4 M ⊙ ). Our GUP parameter upper bound perfectly matches the constraint from $$^{87}$$ 87 Rb cold-atom-recoil experiment. If we consider that the same strength from the additional logarithmic term in the entropy from both GUP and SL model are dependent, for $$\beta < 2\times 10^{-7}$$ β < 2 × 10 - 7 MeV$$^{-2}$$ - 2 , it is clear that SL parameter lower bound is $${\tilde{c}} > -16\times 10^{-34}$$ c ~ > - 16 × 10 - 34 m$$^2$$ 2 . The magnitude of this bound is $$10^{-40}$$ 10 - 40 smaller than the upper bound magnitude of SL parameter considering as independent parameter i.e., $${\tilde{c}} \le 10^7$$ c ~ ≤ 10 7 m$$^2$$ 2 .

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Tensor and isovector–isoscalar terms of relativistic mean field model: Impacts on neutron-skin thickness, charge radius, and nuclear matter

Liliani,

Nugraha,

Diningrum

et al. 2024

Nuclear Physics A

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Tensor and Coulomb-exchange terms in the relativistic mean-field model with δ -meson and isoscalar-isovector coupling

Cited by 5 publications

References 108 publications

Role of Isovector-Isoscalar Coupling on Charge Radius of Heavy and Superheavy Nuclei

Role of Isovector-Isoscalar Coupling on Charge Radius of Heavy and Superheavy Nuclei

Minimal length, nuclear matter, and neutron stars

Tensor and isovector–isoscalar terms of relativistic mean field model: Impacts on neutron-skin thickness, charge radius, and nuclear matter

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