New 
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 Stellar Decay Rate with Implications for the 
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Gao, B. S.; Giraud, S.; Li, K. A.; Sieverding, André; Zegers, R. G. T.; Tang, Xiaodong; Ash, John; Ayyad-Limonge, Y.; Bazin, D.; Biswas, S.; Brown, B. A.; Chen, J.; DeNudt, M.; Farris, P.; Gabler, J. -M.; Gade, A.; Ginter, T. N.; Grinder, M.; Heger, Alexander; Hultquist, C.; Hill, A. M.; Iwasaki, H.; Kwan, E.; Li, J.; Longfellow, B.; Maher, Cavan; Ndayisabye, F.; Noji, S.; Pereira, J.; Qi, Chong; Rebenstock, J.; Revel, A.; Rhodes, D.; Sánchez, A. Martín; Schmitt, J.; Sumithrarachchi, C.; Sun, B. H.; Weißhaar, D.

doi:10.1103/physrevlett.126.152701

Cited by 7 publications

(4 citation statements)

References 44 publications

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“…The 59 Fe(571 keV) state had been assigned a spin/parity of 3/2 − from a (n,p) experiment, while a γ multiplicity measurement (Deacon et al, 2007) prefers a 5/2 − assignment of this state; then this state could also decay via an allowed transition to the 59 Co ground state, and contribute to the stellar β decay of 59 Fe. A high-resolution measurement of the 59 Fe(t, 3 He) 59 Co reaction, performed at NSCL (Gao et al, 2021), found the stellar decay rate to be 3.5 (1.1) times faster than the LMP rate, confirming previous shell model calculations (Li et al, 2016), and the contribution of 571keV could be neglected (although its J π was still not confirmed). Stellar-evolution calculations show that the 60 Fe production of an 18 M star is decreased by 40% when using the new rate (Gao et al, 2021).…”

Section: Reaction Rate Uncertainties Related To 60 Fementioning

confidence: 61%

“…A high-resolution measurement of the 59 Fe(t, 3 He) 59 Co reaction, performed at NSCL (Gao et al, 2021), found the stellar decay rate to be 3.5 (1.1) times faster than the LMP rate, confirming previous shell model calculations (Li et al, 2016), and the contribution of 571keV could be neglected (although its J π was still not confirmed). Stellar-evolution calculations show that the 60 Fe production of an 18 M star is decreased by 40% when using the new rate (Gao et al, 2021).…”

Section: Reaction Rate Uncertainties Related To 60 Fementioning

confidence: 61%

See 1 more Smart Citation

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.

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Section: Reaction Rate Uncertainties Related To 60 Fementioning

confidence: 61%

Section: Reaction Rate Uncertainties Related To 60 Fementioning

confidence: 61%

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

View full text Add to dashboard Cite

show abstract

“…This uncertainty has been eliminated recently by an IMP-NSCL collaboration. Their experimental result shows the 60 Fe yield would be reduced by using the new rate, alleviating the tension between some model predictions and the observation [216]. The 59 Fe(n,γ ) 60 Fe was re-studied by the CIAE and JAEA collaboration using the surrogate method.…”

Section: Radioactive Tracers Of the Galaxymentioning

confidence: 99%

Progress in nuclear astrophysics of east and southeast Asia

Aziz

Ahmad²,

Ahn³

et al. 2021

AAPPS Bull.

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Nuclear astrophysics is an interdisciplinary research field of nuclear physics and astrophysics, seeking for the answer to a question, how to understand the evolution of the universe with the nuclear processes which we learn. We review the research activities of nuclear astrophysics in east and southeast Asia which includes astronomy, experimental and theoretical nuclear physics, and astrophysics. Several hot topics such as the Li problems, critical nuclear reactions and properties in stars, properties of dense matter, r-process nucleosynthesis, and ν-process nucleosynthesis are chosen and discussed in further details. Some future Asian facilities, together with physics perspectives, are introduced.

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“…Stellar EC rates can be theoretically determined following the pioneering works by Fuller, Fowler, and Newman (FFN) [1][2][3][4], where allowed nuclear transitions (especially the Gamow-Teller transitions in the β + direction) dominate. In principle, the Gamow-Teller (GT) transition-strength distributions can be measured with the modern experimental technique with the charge-exchange (CE) reactions [11,[15][16][17], although the energy resolution is relatively limited at present. One should however keep in mind that stellar electron captures may differ substantially from those which can be studied in laboratory today.…”

Section: Introductionmentioning

confidence: 99%

Description of $^{93}$Nb stellar electron-capture rates by the Projected Shell Model

Wang,

Tan,

et al. 2021

Preprint

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Capture of electrons by nuclei is an important process in stellar environments where excited nuclear states are thermally populated. However, accurate treatment for excited configurations in electron capture (EC) rates has been an unsolved problem for medium-heavy and heavy nuclei. In this work, we take the 93 Nb → 93 Zr EC rates as the example to introduce the Projected-Shell-Model (PSM) in which excited configurations are explicitly included as multi-quasiparticle states. Applying the prevalent assumption that the parent nucleus always stays in its ground state in stellar conditions, we critically compare the obtained PSM results with the recently-measured Gamow-Teller transition data, and with the previous calculations by the conventional shell model and the quasiparticle random-phase approximation. We discuss important ingredients that are required in theoretical models used for stellar EC calculations, and demonstrate effects of the explicit inclusion of excited nuclear states in EC rate calculations, especially when both electron density and environment temperature are high.

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New Fe59 Stellar Decay Rate with Implications for the Fe60

Cited by 7 publications

References 44 publications

The Radioactive Nuclei $^{\textbf{26}}$Al and $^{\textbf{60}}$Fe 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

Progress in nuclear astrophysics of east and southeast Asia

Description of $^{93}$Nb stellar electron-capture rates by the Projected Shell Model

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