Positive Parity Levels of 21,23Na Isotopes by Using the Nuclear Shell

Hasan, Ali K.; Obeed, Fatema H.; Rahim, A. N.

doi:10.15407/ujpe65.1.3

Cited by 6 publications

(6 citation statements)

References 14 publications

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“…The comparison of experimental and theoretical values of reduced M1 matrix elements, |M(M1)| = √ (2J i + 1)B(M1), is presented in Fig. 2 for transitions in 23 Mg and 21,23 Na [30]. Optimum effective g-factors USDA(6) and USDB (6) from Table I of Ref.…”

Section: Nuclear Structure Considerationsmentioning

confidence: 99%

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Understanding the cosmic abundance of ²²Na: Lifetime measurements in ²³Mg

Fougères¹,

Santos²,

Смирнова³

et al. 2023

EPJ Web Conf.

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Simulations of explosive nucleosynthesis in novae predict the production of 22Na, a key astronomical observable to constrain nova models. Its gamma-ray line at 1.275 MeV has not yet been observed by the gamma-ray space telescopes. The 20Ne/22Ne ratio in presolar grains, a possible tool to identify nova grains, also depends on 22Na produced. Uncertainties on its yield in classical novae currently originate from the rate of the 22Na(p, γ)23Mg reaction. At peak novae temperatures, this reaction is dominated by a resonance at ER=0.204 MeV, corresponding to the Ex=7.785 MeV excited state in 23Mg. The resonance strengths measured so far disagree by one order of magnitude. An experiment has been performed at GANIL to measure the lifetime and the proton branching ratio of this key state, with a femtosecond resolution for the former. The reactions populating states in 23Mg have been studied with a high resolution detection set-up, i.e. the particle VAMOS, SPIDER and gamma tracking AGATA spectrometers, allowing the measurements of lifetimes and proton branchings. We present here a comparison between experimental results and shell-model calculations, that allowed us to assign the spin and parity of the key state. Rather small values obtained for reduced M1 matrix elements, M(M1) ≲ 0.5 µN, and proton spectroscopic factors, C2Sp<10−2, seem to be beyond the accuracy of the shell model. With the reevaluated 22Na(p, γ)23Mg rate, the 22Na detectability limit and its observation frequency from novae are found promising for the future space telescopes.

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Section: Nuclear Structure Considerationsmentioning

confidence: 99%

“…Figure 2. Correlation between measured and theoretical reduced matrix elements |M(M1)| values for transitions in23 Mg and21,23 Na[30]. Theoretical values were obtained from sd-shell calculations with USDAcpn and USDBcpn[25,26], experimental ones from measured (τ, E γ,0 ), resulting in rms=0.322 µ N (USDAcpn) and rms=0.273 µ N (USDBcpn).…”

mentioning

confidence: 99%

Understanding the cosmic abundance of ²²Na: Lifetime measurements in ²³Mg

Fougères¹,

Santos²,

Смирнова³

et al. 2023

EPJ Web Conf.

View full text Add to dashboard Cite

show abstract

“…Among these models, the accomplished nuclear shell model stands out. This model identifies the energy states, their placements, and the transitions occurring between those states, thereby providing a significant portrayal of nuclear attributes [2,3]. In the realm of shell-model calculations, there are two primary components: the interaction between nucleons (N-N interaction) and the configuration space allotted for valence particles.…”

Section: Introductionmentioning

confidence: 99%

Calculation of Energy Levels B(E2) and B(M1) for 58,59Cu Isotopes by Using NushellX@MSU Code

Hasan,

Abed

2024

Ukr. J. Phys.

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In this study, the NushellX@MSU code was applied to compute energy levels, B(E2) and B(M1), values for 58Cu and 59Cu isotopes, using the jj44pn shell and the jun45pn effective interaction. The model space encompassed all possible nucleon configurations within the (f5/2, p3/2, p1/2, and g9/2) orbits. Overall, the computed probabilities of electromagnetic transitions and energy levels for the 58Cu and 59Cu isotopes demonstrate a reasonable consistency with available experimental data.

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“…Fatema H. Obeed and Baneen S. Abed, used the surface delta and modified surface delta interactions by applying the nuclear shell model to calculate values of excitation energies for isotopes of equal mass number containing two nucleons outside the closed core 114 Sn, these nuclei are; the isotope (Tin) 116 Sn contains two neutrons within the model space (3s1/2, 2d3/2, 1h11/2) and the other isotope is 116 Te (Tellurium) contains two protons within the model space (1g7/2, 2d5/2, 3s1/2, 2d3/2, 1h11/2) [10]. A. K. Hasan et al, investigated on the energy levels and transition probabilities 𝐵 (𝐸2; ↓) and 𝐵 (𝑀1; ↓) for 21,23 Na isotopes by using the (USDA and USDB) interactions in the (𝑠𝑑-shell) model space [11]. S. Akkoyun, investigated the nuclear structure properties of A=49 isobars, the double-magic 40 Ca nucleus was considered an inert core, and fp model space was taken into account for the valance nucleons [12].…”

Section: Introductionmentioning

confidence: 99%

Hole-Hole Collective Excitations in 106, 112, 130Sn Isotopes

Saber,

Taqi

2023

East Eur. J. Phys.

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In this paper, energy-level schemes of neutron rich and reduced electric transition strengths of Tin isotopes 106Sn, 112Sn and 130Sn were studied using collective models, i.e., hole-hole Tamm-Dancoff Approximation (hh TDA) and hole-hole Random Phase Approximation (hh RPA). According to these models, the excited states of closed core A-2 systems with multipolarity J and isospin T can be described as a linear combination of hole-hole (hh) pairs. Therefore, in our approach, the low-lying states of the investigated isotopes 106Sn, 112Sn and 130Sn are obtained by acting two-hole operators on a correlated core 108Sn, 114Sn and 132Sn, respectively. The Hamiltonian is diagonalized within the model space include {1g7/2, 2d5/2, 2d3/2, 3s1/2 and 1h11/2} orbits, using the matrix elements of neutron-neutron (N-N) interaction and modified surface delta interaction (MSDI). The hh TDA and hh RPA are checked by using the resultant eigenvalues and eigenvectors to calculate the excitation energies and reduced electric transition strengths. A comparison had been made between our theoretical predictions and the recent available experimental data. Reasonable agreements were obtained from these comparisons.

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Positive Parity Levels of 21,23Na Isotopes by Using the Nuclear Shell

Cited by 6 publications

References 14 publications

Understanding the cosmic abundance of ²²Na: Lifetime measurements in ²³Mg

Understanding the cosmic abundance of ²²Na: Lifetime measurements in ²³Mg

Calculation of Energy Levels B(E2) and B(M1) for 58,59Cu Isotopes by Using NushellX@MSU Code

Hole-Hole Collective Excitations in 106, 112, 130Sn Isotopes

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Positive Parity Levels of 21,23Na Isotopes by Using the Nuclear Shell

Cited by 6 publications

References 14 publications

Understanding the cosmic abundance of 22Na: Lifetime measurements in 23Mg

Understanding the cosmic abundance of 22Na: Lifetime measurements in 23Mg

Calculation of Energy Levels B(E2) and B(M1) for 58,59Cu Isotopes by Using NushellX@MSU Code

Hole-Hole Collective Excitations in 106, 112, 130Sn Isotopes

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Understanding the cosmic abundance of ²²Na: Lifetime measurements in ²³Mg

Understanding the cosmic abundance of ²²Na: Lifetime measurements in ²³Mg