Decay of the key 92-keV resonance in the 25Mg(p,γ) reaction to the ground and isomeric states of the cosmic γ-ray emitter 26Al

Kankainen, A.; Woods, P. J.; Doherty, D. T.; Albers, H. M.; Albers, M.; Ayangeakaa, A. D.; Carpenter, M. P.; Chiara, C. J.; Harker, J.; Janssens, R. V. F.; Lederer-Woods, C.; Seweryniak, D.; Strieder, F.; Zhu, S.

doi:10.1016/j.physletb.2020.136033

Cited by 7 publications

(21 citation statements)

References 20 publications

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“…However, the latter was based on simulations of BGO summing data and was lower than an earlier value of 0.80 ± 0.15 obtained in a 24 Mg( 3 He, p) study [17]. More recently, Kankainen et al performed a high-resolution γ -ray spectroscopy study of the 93-keV resonance using the Gammasphere array [18]. In that work [18], the 24 Mg( 3 He, p) light-ion fusion reaction was used to populate proton-unbound levels in 26 Al and four γdecay branches from the 93-keV resonance were observed at 1256.4 (13), 3238.7 (20), 4326.9 (20), and 4638.0(21) keV, respectively.…”

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confidence: 86%

“…Intriguingly, in Ref. [18], the 4327-keV γ ray, which decays to the 2 + 2 state in 26 Al and strongly feeds the isomeric level, was found to represent the most intense decay branch of the 93-keV resonance-it is largely due to this fact that Kankainen et al obtained a f 0 value at the lower end of all previously adopted values [16,17,19,20].…”

mentioning

confidence: 96%

“…More recently, Kankainen et al performed a high-resolution γ -ray spectroscopy study of the 93-keV resonance using the Gammasphere array [18]. In that work [18], the 24 Mg( 3 He, p) light-ion fusion reaction was used to populate proton-unbound levels in 26 Al and four γdecay branches from the 93-keV resonance were observed at 1256.4 (13), 3238.7 (20), 4326.9 (20), and 4638.0(21) keV, respectively. An angular distribution analysis of the 3239and 4327-keV γ rays indicated a 2 − spin-parity assignment for the 93-keV resonance and the observed γ -ray intensities established a ground-state branching fraction of f 0 = 0.52 ± 0.02(stat.)…”

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confidence: 99%

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Revised decay properties of the key 93-keV resonance in the Mg25(p,γ) reaction and its influence on the MgAl cycle in astrophysical environments

et al. 2022

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Revised decay properties of the key 93-keV resonance in the Mg25(p,γ) reaction and its influence on the MgAl cycle in astrophysical environments

et al. 2022

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“…= 92 and 198 keV, have been measured using the LUNA underground facility with its accelerator (Strieder et al 2012). However, due to the lack of statistical precision of the measurement and of decay transition information, the branching ratio of the ground state transition still holds a rather large uncertainty, in spite of some progress from a recent measurement with Gammasphere at Argonne National Laboratory (ANL) (Kankainen et al 2021). Prospects to re-study this resonance with better statics are offered by the new JUNA facility in China, also extending the measurements down to the resonance at 58 keV with a more intense beam (Liu et al 2016).…”

Section: Uncertainties In the Relevant Reaction Ratesmentioning

confidence: 99%

The radioactive nuclei and in the Cosmos and in the solar system

Diehl

Lugaro

Heger

et al. 2021

Publ. Astron. Soc. Aust.

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The cosmic evolution of the chemical elements from the Big Bang to the present time is driven by nuclear fusion reactions inside stars and stellar explosions. A cycle of matter recurrently re-processes metal-enriched stellar ejecta into the next generation of stars. The study of cosmic nucleosynthesis and this matter cycle requires the understanding of the physics of nuclear reactions, of the conditions at which the nuclear reactions are activated inside the stars and stellar explosions, of the stellar ejection mechanisms through winds and explosions, and of the transport of the ejecta towards the next cycle, from hot plasma to cold, star-forming gas. Due to the long timescales of stellar evolution, and because of the infrequent occurrence of stellar explosions, observational studies are challenging, as they have biases in time and space as well as different sensitivities related to the various astronomical methods. Here, we describe in detail the astrophysical and nuclear-physical processes involved in creating two radioactive isotopes useful in such studies, $^{26}\mathrm{Al}$ and $^{60}\mathrm{Fe}$ . Due to their radioactive lifetime of the order of a million years, these isotopes are suitable to characterise simultaneously the processes of nuclear fusion reactions and of interstellar transport. We describe and discuss the nuclear reactions involved in the production and destruction of $^{26}\mathrm{Al}$ and $^{60}\mathrm{Fe}$ , the key characteristics of the stellar sites of their nucleosynthesis and their interstellar journey after ejection from the nucleosynthesis sites. This allows us to connect the theoretical astrophysical aspects to the variety of astronomical messengers presented here, from stardust and cosmic-ray composition measurements, through observation of $\gamma$ rays produced by radioactivity, to material deposited in deep-sea ocean crusts and to the inferred composition of the first solids that have formed in the Solar System. We show that considering measurements of the isotopic ratio of $^{26}\mathrm{Al}$ to $^{60}\mathrm{Fe}$ eliminate some of the unknowns when interpreting astronomical results, and discuss the lessons learned from these two isotopes on cosmic chemical evolution. This review paper has emerged from an ISSI-BJ Team project in 2017–2019, bringing together nuclear physicists, astronomers, and astrophysicists in this inter-disciplinary discussion.

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“…=92 and 198 keV, have been measured using the LUNA underground facility with its accelerator (Strieder et al, 2012). However, due to the lack of statistical precision of the measurement and of decay transition information, the branching ratio of the ground state transition still holds a rather large uncertainty, in spite of some progress from a recent measurement with Gammasphere at ANL (Kankainen et al, 2021). Prospects to re-study this resonance with better statics are offered by the new JUNA facility in China, also extending the measurements down to the resonance at 58 keV with a more intense beam (Liu et al, 2016).…”

Section: Uncertainties In the Relevant Reaction Ratesmentioning

confidence: 99%

The Radioactive Nuclei $^{\textbf{26}}$Al and $^{\textbf{60}}$Fe in the Cosmos and in the Solar System

Diehl,

Lugaro,

Heger

et al. 2021

Preprint

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The cosmic evolution of the chemical elements from the Big Bang to the present time is driven by nuclear fusion reactions inside stars and stellar explosions. A cycle of matter recurrently re-processes metal-enriched stellar ejecta into the next generation of stars. The study of cosmic nucleosynthesis and of this matter cycle requires the understanding of the physics of nuclear reactions, of the conditions at which the nuclear reactions are activated inside the stars and stellar explosions, of the stellar ejection mechanisms through winds and explosions, and of the transport of the ejecta towards the next cycle, from hot plasma to cold, star-forming gas. Due to the long timescales of stellar evolution, and because of the infrequent occurrence of stellar explosions, observational studies are challenging, as they have biases in time and space as well as different sensitivities related to the various astronomical methods. Here, we describe in detail the astrophysical and nuclear-physical processes involved in creating two radioactive isotopes useful in such studies, 26 Al and 60 Fe. Due to their radioactive lifetime of the order of a million years these isotopes are suitable to characterise simultaneously the processes of nuclear fusion reactions and of interstellar transport. We describe and discuss the nuclear reactions involved in the production and destruction of 26 Al and 60 Fe, the key characteristics of the stellar sites of their nucleosynthesis and their interstellar journey after ejection from the nucleosynthesis sites. This allows us to connect the theoretical astrophysical aspects to the variety of astronomical messengers presented here, from stardust and cosmic-ray composition measurements, through observation of γ rays produced by radioactivity, to material deposited in deep-sea ocean crusts and to the inferred composition of the first solids that have formed in the Solar System. We show that considering measurements of the isotopic ratio of 26 Al to 60 Fe eliminate some of the unknowns when interpreting astronomical results, and discuss the lessons learned from these two isotopes on cosmic chemical evolution. This review paper has emerged from an ISSI-BJ Team project in 2017-2019, bringing together nuclear physicists, astronomers, and astrophysicists in this inter-disciplinary discussion.

show abstract

Decay of the key 92-keV resonance in the 25Mg(p,γ) reaction to the ground and isomeric states of the cosmic γ-ray emitter 26Al

Cited by 7 publications

References 20 publications

Revised decay properties of the key 93-keV resonance in the Mg25(p,γ) reaction and its influence on the MgAl cycle in astrophysical environments

Revised decay properties of the key 93-keV resonance in the Mg25(p,γ) reaction and its influence on the MgAl cycle in astrophysical environments

The radioactive nuclei and in the Cosmos and in the solar system

The Radioactive Nuclei $^{\textbf{26}}$Al and $^{\textbf{60}}$Fe in the Cosmos and in the Solar System

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