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

Abstract

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 stars; to massive and very massive stars, both their Wolf-Rayet 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.

Metadata

Item Type:	Article
Authors/Creators:	Laird, A. M. https://orcid.org/0000-0003-0423-363X Lugaro, M. Kankainen, A. Adsley, P. Bardayan, D. W. Brinkman, H. E. Côté, B. Deibel, C. M. Diehl, R. Hammache, F. den Hartogh, J. W. José, J. Kurtulgil, D. Lederer-Woods, C. Lotay, G. Meynet, G. Palmerini, S. Pignatari, M. Reifarth, R. de Séréville, N. Sieverding, A. Stancliffe, R. J. Trueman, T. C.L. Lawson, T. Vink, J. S. Massimi, C. Mengoni, A.
Copyright, Publisher and Additional Information:	Funding Information: This paper is based upon work from the ‘ChETEC’ COST Action (CA16117), supported by COST (European Cooperation in Science and Technology) and the National Science Foundation under Grant No. OISE-1927130 (IReNA). AML also acknowledges support from STFC (Science and Technology Facilities Council). PA thanks the trustees and staff of the Claude Leon Foundation for support in the form of a postdoctoral fellowship. MP acknowledges the support of NuGrid, JINA-CEE (NSF Grant PHY-1430152) and STFC (through the University of Hulls Consolidated Grant ST/R000840/1), and ongoing access to viper , the University of Hull High Performance Computing Facility. MP acknowledges the support from the ‘Lendület-2014’ Programme of the Hungarian Academy of Sciences (Hungary). BC acknowledges the support from the ERC Consolidator Grant (Hungary) funding scheme (Project RADIOSTAR, G.A. n. 724 560), the Hungarian Academy of Sciences via the Lendület project LP2014-17, and the National Science Foundation (NSF, USA) under Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). RR and DK are thankful for support from BMBF 05P19RFFN1 and the European Research Council under the European Unions's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement N. 615126. AK acknowledges the funding from the European Unions Horizon 2020 research and innovation program under grant agreement No. 771036 (ERC CoG MAIDEN). DB acknowledges support from the National Science Foundation under grants PHY-2011890 (University of Notre Dame), PHY-1430152 (JINA Center for the Evolution of the Elements), and OISE-1927130 (International Research Network for Nuclear Astrophysics). CLW acknowledges support from the UK Science and Technologies Facilities Council (STFC), projects ST/P004008/1 and ST/M006085/1, and the European Research Council ERC-2015-STG Nr. 677 497. AS acknowledges support from the U.S. Department of Energy through grant DE-FG02-87ER40328 (UM). JJ acknowledges support by the Spanish MINECO Grant PID2020-117252GB-I00, by the E.U. FEDER funds, and by the AGAUR/Generalitat de Catalunya grant SGR-661/2017. Finally, we thank the ChETEC-INFRA project funded from the European Unions Horizon 2020 research and innovation programme under Grant agreement No 101008324. Publisher Copyright: © 2023 The Author(s). Published by IOP Publishing Ltd.
Keywords:	nuclear reaction rate,nucleosynthesis,radioisotope
Dates:	Published: 28 February 2023 Accepted: 24 October 2022
Institution:	The University of York
Academic Units:	The University of York > Faculty of Sciences (York) > Physics (York) The University of York > Faculty of Sciences (York)
Funding Information:	Funder Grant number SCIENCE AND TECHNOLOGY FACILITIES COUNCIL (STFC) ST/V001035/1 SCIENCE AND TECHNOLOGY FACILITIES COUNCIL (STFC) ST/P003885/1
Depositing User:	Pure (York)
Date Deposited:	12 Jan 2024 09:50
Last Modified:	22 Jan 2025 00:23
Published Version:	https://doi.org/10.1088/1361-6471/ac9cf8
Status:	Published
Refereed:	Yes
Identification Number:	10.1088/1361-6471/ac9cf8
Related URLs:	http://www.scopus.com/inward/record.url?...
Open Archives Initiative ID (OAI ID):	oai:eprints.whiterose.ac.uk:207515

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

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