The nuclear ground-state properties and stellar electron emission rates of 76Fe, 78Ni, 80Zn, 126Ru, 128Pd and 130Cd using RMF and pn-QRPA models

Nabi, Jameel-Un; Bayram, Tuncay; Daraz, Gul; Kabir, Abdul; Şentürk, Şevki

doi:10.1016/j.nuclphysa.2021.122278

Cited by 8 publications

(3 citation statements)

References 68 publications

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“…In figure 2, we show the comparisons of the semi-empirical (F 1 , F 2 , F 3 , F 4 ) and macro-microscopic (FRDM +QRPA) [35] calculations to the estimations using self-consistent models (Gross theory + Hartree-Fock-Bogoliubov (GT-HFB) [66,67], density functional continuum quasiparticle random phase approximation (DF-CQRPA) [67][68][69], proton-neutron relativistic quasiparticle random phase approximation (pnRQRPA) [70], large scale shell model (LSSM) [71,72], shell model (SM) [72,73], proton-neutron relativistic quasiparticle timeblocking approximation (pnRQTBA) [70], and finite Fermi system theory (FFST) [74]), where available, for the 66−76 Fe (panel A), 68−78 Ni (panel B), and 119−127 Rh (panel C) isotopes. It was found that the difference between the semi-empirical calculations and self-consistent-model estimations is small, which is from a few factors to one order of magnitude, except for the pnRQRPA model.…”

Section: 139mentioning

confidence: 99%

Beta-decay half-lives of the isotopes close to the neutron drip line and astrophysical implications

Quyen¹,

Chae²,

Uyen³

et al. 2022

Phys. Scr.

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In this paper, we examined the β--decay half-lives of 94 extremely neutron-rich isotopes with Z = 26 − 57 close to the neutron drip line, which are important for the r-process calculations. The half-lives were calculated using four semi-empirical models and compared to those based on the FRDM+QRPA approach and available measured data. The impact of the diﬀerence in the models on the half-life predictions was investigated. We found that theoretical calculations for the β-decay half-life have a large deviation, up to 60%, which is mostly similar to that in measurements. The half-lives of the investigated nuclei are ranging from a few to hundreds of milliseconds. The r-process abundances in various astrophysical scenarios were calculated by using the predicted half-lives. The half-life uncertainty due to diﬀerent models results in a large deviation in the isotopic abundance, specially for the isotopes in the mass range of A > 210. The shell closures in 76Fe is still a doubt due to the discrepancy in the trends of the half-life and paring gap while a closed-shell at N = 82 in 127Rh is possible. The results of this study also notice that it is a challenge for measuring precisely the masses of 106Rb, 116,117Nb, 122Tc, and 128Rh because of their short half-lives.

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Section: 139mentioning

confidence: 99%

Beta-decay half-lives of the isotopes close to the neutron drip line and astrophysical implications

Quyen¹,

Chae²,

Uyen³

et al. 2022

Phys. Scr.

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“…The observed peaks in the abundance pattern of r-process elements arise due to the deceleration of matter flow at these WPs. Thus, matter assembles at the WP, and nuclei undergo a series of BDs before the r-process recommences [2,[10][11][12][13][14][15][16]. The high temperature (> 1 GK) and high neutron density (> 10 20 g/cm 3 ) conditions associated with the neutron-star to neutron-star collisions [17] and core-collapse supernovae (CCSNe) [11] establish a site for creating the r-process elements.…”

Section: Introductionmentioning

confidence: 99%

Impact of the Brink-Axel hypothesis on unique first-forbidden β-transitions for r-process nuclei*

Farooq,

Nabi,

Shehzadi

2024

Chinese Phys. C

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Key nuclear inputs for the astrophysical r-process simulations are the weak interaction rates. Consequently, the accuracy of these inputs directly affects the reliability of nucleosynthesis modeling. Majority of the stellar rates, used in simulation studies, are calculated invoking the Brink-Axel (BA) hypothesis. The BA hypothesis assumes that the strength functions of all parent excited states are the same as for the ground state, only shifted in energies. However, BA hypothesis has to be tested against microscopically calculated state-by-state rates. In this project we study the impact of the BA hypothesis on calculated stellar β--decay and electron capture rates. Our investigation include both Unique First Forbidden (U1F) and allowed transitions for 106 neutron-rich trans-iron nuclei ([27, 77] ≤ [Z, A] ≤ [82, 208]). The calculations were performed using the deformed proton-neutron quasi-particle random-phase approximation (pn-QRPA) model with a simple plus quadrupole separable and schematic interaction. Waiting-point and several key r-process nuclei lie within the considered mass region of the nuclear chart. We computed electron capture and β--decay rates using two different prescriptions for strength functions. One was based by invoking BA hypothesis and the other was the state-by-state calculation of strength functions, under stellar density and temperature conditions ([10, 1] ≤ [ρYe(g/cm3), T(GK)] ≤ [1011, 30]). Our results show that BA hypothesis invoked U1F β-− rates are overestimated by 4–5 orders of magnitude as compared to microscopic rates. For capture rates, more than 2 orders of magnitude difference was noted when applying BA hypothesis. It was concluded that the BA hypothesis is not a reliable approximation, especially for the β--decay forbidden transitions.

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“…Afterwards, this model has been implemented by Nabi et al [25] for weak rates calculations of neutron-rich isotopes of several elements having A 100. In his recent publications, Nabi et al presented β-decay half-lives, GT strength distributions, phase space and stellar weak rates of waiting point nuclei having N = 50, 82 [26,27] and N = 126 [28] by employing the deformed p-n-QRPA model. The β-decay properties of even-even chromium isotopes were earlier studied using the same model [29].…”

Section: Introductionmentioning

confidence: 99%

β-Decay properties of neutron-rich yttrium isotopes

Farooq¹,

Nabi²,

Shehzadi³

2021

Phys. Scr.

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In this study, we have reported key nuclear properties of weak β-decay processes on Yttrium isotopes for the mass number range A = 101 − 108. This mass region has importance while dealing with astrophysical r-process abundances. Our study might be helpful in r-process simulations. We have computed charge-changing strength distributions, β-decay half-lives, β-delayed neutron emission probabilities and β − (EC) weak rates under stellar conditions. We have performed microscopic calculations based on deformed proton-neutron quasi-particle random phase approximation (p-n-QRPA) over a wide temperature (10 7 − 3 × 10 10 ) K and density (10 − 10 11 ) g/cm 3 domain. Unique first-forbidden (U1F) transitions have been included in the calculations in addition to the allowed transitions. A significant decrease in calculated half-lives in ceratin cases, e.g., in 107 Y ( 108 Y) by about 67% (42%), has been observed because of the contribution from U1F transitions. We have compared present results with measured and theoretical works. A good agreement of our half-lives with experimental data is observed.

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The nuclear ground-state properties and stellar electron emission rates of 76Fe, 78Ni, 80Zn, 126Ru, 128Pd and 130Cd using RMF and pn-QRPA models

Cited by 8 publications

References 68 publications

Beta-decay half-lives of the isotopes close to the neutron drip line and astrophysical implications

Beta-decay half-lives of the isotopes close to the neutron drip line and astrophysical implications

Impact of the Brink-Axel hypothesis on unique first-forbidden β-transitions for r-process nuclei*

β-Decay properties of neutron-rich yttrium isotopes

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