Revised decay properties of the key 93-keV resonance in the 
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 reaction and its influence on the MgAl cycle in astrophysical environments

Lotay, G.; Doherty, D. T.; Janssens, R. V. F.; Seweryniak, D.; Albers, H. M.; Carpenter, M. P.; Champagne, A. E.; Chiara, C. J.; Hoffman, C. R.; Iliadis, Christian; Kankainen, A.; Lauritsen, T.; Zhu, S.

doi:10.1103/physrevc.105.l042801

Cited by 4 publications

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“…± 0.06 (syst.) [186] to f 0 = 0.76 (10) [189]. Similarly, on the basis of the γ-ray branching information stored in the ENSDF database, the f 0 value for the astrophysically unimportant E r = 109 keV resonance has values ranging from f 0 = 0.0041 (7) to f 0 = 0.71 depending on the source.…”

Section: E X (Kev)mentioning

confidence: 99%

“…The decrease in the reaction rate at T ≈ 0.1 GK is due to the updated resonance strength of the 93 keV resonance from LUNA and JUNA [187,188]. The resonance strength and ground state branching fraction for the E r = 93 keV resonance are weighted averages of [187,188] and [188,189], respectively. 26 Al(p, γ) 27 Si Proton capture on 26 Al provides the main destruction mechanism for 26 Al in several stellar sites such as classical novae, convective core hydrogen burning in massive stars, and hydrogen burning in intermediate-mass AGB stars.…”

Section: E X (Kev)mentioning

confidence: 99%

“…The decrease in the reaction rate at low temperatures is due to the shifted resonance energy computed, taking the atomic binding into account. The difference at T ≈ 0.1 GK is due to the updated information on the E r = 93 keV resonance from [187][188][189]. [214].…”

Section: The Destruction Reactionmentioning

confidence: 99%

mentioning

confidence: 99%

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Progress on nuclear reaction rates affecting the stellar production of ²⁶Al

Laird

Lugaro

Kankainen

et al. 2023

J. Phys. G: Nucl. Part. Phys.

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The radioisotope 26Al is a key observable for nucleosynthesis in the Galaxy and the environment of the early Solar System. To properly interpret the large variety of astronomical and meteoritic data, it is crucial to understand both the nuclear reactions involved in the production of 26Al in the relevant stellar sites and the physics of such sites. These range from the winds of low- and intermediate-mass asymptotic giant branch (AGB) stars; to massive and very massive stars, both their Wolf-Rayet (WR) winds and their final core-collapse supernovae (CCSN); and the ejecta from novae, the explosions that occur on the surface of a white dwarf accreting material from a stellar companion. Several reactions affect the production of 26Al in these astrophysical objects, including (but not limited to) 25Mg(p,γ)26Al, 26Al(p,γ)27Si, and 26Al(n,p/α). Extensive experimental effort has been spent during recent years to improve our understanding of such key reactions. Here we present a summary of the astrophysical motivation for the study of 26Al, a review of its production in the different stellar sites, and a timely evaluation of the currently available nuclear data. We also provide recommendations for the nuclear input into stellar models and suggest relevant, future experimental work.

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