Unique first-forbidden β-decay transitions in odd–odd and even–even heavy nuclei

Nabi, Jameel-Un; Çakmak, Necla; Majid, Muhammad; Selam, Cevad

doi:10.1016/j.nuclphysa.2016.07.003

Cited by 9 publications

(4 citation statements)

References 31 publications

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“…The b j j p n , b j j p n appearing above stands for reduced matrix elements of the multipole operators for rank 0, 1 and 2 [15]. Here we have shown only the relevant equations and detailed formalism can be seen from [16,17]. Details of rank 0 excitation computation are available in [18].…”

Section: The Pn-qrpa (Ws) Modelmentioning

confidence: 99%

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β-decay of N = 126 isotones for the r-process nucleosynthesis

Nabi¹,

Çakmak²,

Ullah³

et al. 2021

Phys. Scr.

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The β-decay properties of nuclei with neutron number N = 126 is investigated in this paper. Two different versions of the proton-neutron quasi particle random phase (pn-QRPA) model were employed to compute β-decay rates and half-lives for the N = 126 isotones. The first set of calculation solves the pn-QRPA equations using the schematic model (SM) approach. The Woods-Saxon potential was employed as a mean-field basis. A spherical shape assigned for each waiting point nuclei throughout all simulations. Both allowed Gamow-Teller (GT) and first-forbidden (FF) transitions were considered in the particle-hole (ph) channel. The second set uses the pn-QRPA model in deformed Nilsson basis to calculate β-decay rates for allowed GT and unique first-forbidden (U1F) transitions under terrestrial and stellar conditions. Our results are in agreement with shell model findings that first-forbidden transitions lead to a considerable decrement in the calculated half-lives of the isotones. Inclusion of the first-forbidden contribution led to a decent agreement of our computed terrestrial β-decay half-lives with measured ones, much better than the previous calculations. The possible implication of the waiting point nuclei on r-process nucleosynthesis is discussed briefly.

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Section: The Pn-qrpa (Ws) Modelmentioning

confidence: 99%

“…The pp interaction strength was taken as 0.0001. The functional form of χ is the same as previously used in [16,17,23]. The deformation parameter (β 2 ) was calculated using…”

Section: The Pn-qrpa (N) Modelmentioning

confidence: 99%

β-decay of N = 126 isotones for the r-process nucleosynthesis

Nabi¹,

Çakmak²,

Ullah³

et al. 2021

Phys. Scr.

Self Cite

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“…The selected values of χ and κ exhibited an inverse mass dependence as suggested in Refs. [18,[35][36][37]. Other variables for the capture rates estimation are the pairing gap (∆ p , ∆ n ), nuclear deformation (β 2 ), Q-values and the Nilsson potential parameters (NPP).…”

Section: The Pn-qrpa Modelmentioning

confidence: 99%

“…For necessary formalism of calculation of U1F transitions in the deformed pn-QRPA model with separable interaction, see Refs. [22,36,37]. The large temperature inside the core of massive stars implies that there is a finite chance of occupations of parent excited levels in stellar matter.…”

Section: The Pn-qrpa Modelmentioning

confidence: 99%

Ground-state Nuclear Properties of Neutron-rich Copper Isotopes and Lepton Capture Rates in Stellar Matter

Nabi¹,

Bayram²,

Majid³

2018

Acta Phys. Pol. B

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This study essentially consists of two separate investigations where we study neutron-rich isotopes of copper. Two different nuclear models were selected to perform the two investigations. In the first part of this paper, the nuclear ground-state properties of neutron-rich copper isotopes (72 ≤ A ≤ 82) have been studied with the help of the relativistic mean field (RMF) model. The second portion of this paper is dedicated to calculation of lepton capture rates in stellar environment. Ground and excited states of GT and U1F strength functions were calculated in a microscopic way employing the deformed proton-neutron quasiparticle random phase approximation (pn-QRPA) model. The lepton capture rates were computed on a wide temperature range of (0.01-30)×10 9 K and stellar density range of (10-10 11) g/cm 3. We compared our computed half-lives (GT + U1F) with previous theoretical and measured results. Our calculated terrestrial half-lives agree well with the measured ones. Our study shows that, at high stellar temperatures, allowed GT and, specially, U1F positron capture rates dominate the competing β-decay rates. For a better description of presupernova evolutionary phases of massive stars, simulators are recommended to take into account lepton capture rates on neutron-rich copper isotopes presented in this work.

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