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Destruction of the cosmic γ-ray emitter Al26 in massive stars: Study of the key Al26(n,α) reaction

C. Lederer-Woods1,*, P. J. Woods1, T. Davinson1, A. Estrade1,†, J. Heyse2, D. Kahl1,‡, S. J. Lonsdale1, C. Paradela2, P. Schillebeeckx2 et al. (n_TOF Collaboration)

P. Schillebeeckx2, O. Aberle3, S. Amaducci4,5, J. Andrzejewski6, L. Audouin7, M. Bacak8,3,9, J. Balibrea10, M. Barbagallo11, F. Bečvář12, E. Berthoumieux9, J. Billowes13, D. Bosnar14, A. Brown15, M. Caamaño16, F. Calviño17, M. Calviani3, D. Cano-Ott10, R. Cardella3, A. Casanovas17, F. Cerutti3, Y. H. Chen7, E. Chiaveri3,13,18, N. Colonna11, G. Cortés17, M. A. Cortés-Giraldo18, L. Cosentino19, S. Cristallo20,21, L. A. Damone11,22, M. Diakaki9, C. Domingo-Pardo23, R. Dressler24, E. Dupont9, I. Durán16, B. Fernández-Domínguez16, A. Ferrari3, P. Ferreira25, F. J. Ferrer26,27, P. Finocchiaro19, V. Furman28, K. Göbel29, A. R. García10, A. Gawlik6, S. Gilardoni3, T. Glodariu29,†, I. F. Gonçalves25, E. González-Romero10, E. Griesmayer8, C. Guerrero18, F. Gunsing9,3, H. Harada31, S. Heinitz24, D. G. Jenkins15, E. Jericha8, F. Käppeler32, Y. Kadi3, A. Kalamara33, P. Kavrigin8, A. Kimura31, N. Kivel24, M. Kokkoris33, M. Krtička12, D. Kurtulgil29, E. Leal-Cidoncha16, H. Leeb8, J. Lerendegui-Marco18, S. Lo Meo34,4, D. Macina3, A. Manna4,5, J. Marganiec6,35, T. Martínez10, A. Masi3, C. Massimi4,5, P. Mastinu36, M. Mastromarco11, E. A. Maugeri24, A. Mazzone11,37, E. Mendoza10, A. Mengoni34, P. M. Milazzo38, F. Mingrone3, A. Musumarra19,39, A. Negret30, R. Nolte35, A. Oprea30, N. Patronis40, A. Pavlik41, J. Perkowski6, I. Porras42, J. Praena42, J. M. Quesada18, D. Radeck35, T. Rauscher43,44, R. Reifarth29, C. Rubbia3, J. A. Ryan13, M. Sabaté-Gilarte3,18, A. Saxena45, D. Schumann24, P. Sedyshev28, A. G. Smith13, N. V. Sosnin13, A. Stamatopoulos33, G. Tagliente11, J. L. Tain23, A. Tarifeño-Saldivia17, L. Tassan-Got7, S. Valenta12, G. Vannini4,5, V. Variale11, P. Vaz25, A. Ventura4, V. Vlachoudis3, R. Vlastou33, A. Wallner46, S. Warren13, C. Weiss8, T. Wright13, and P. Žugec14,3 (n_TOF Collaboration)

  • 1School of Physics and Astronomy, University of Edinburgh, Peter Guthrie Tait Road, EH9 3FD Edinburgh, United Kingdom
  • 2European Commission, Joint Research Centre, Geel, Retieseweg 111, B-2440 Geel, Belgium
  • 3European Organization for Nuclear Research (CERN), Switzerland
  • 4Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Italy
  • 5Dipartimento di Fisica e Astronomia, Università di Bologna, Italy
  • 6University of Lodz, Poland
  • 7Institut de Physique Nucléaire, CNRS-IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay Cedex, France
  • 8Technische Universität Wien, Austria
  • 9CEA Irfu, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
  • 10Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
  • 11Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Italy
  • 12Charles University, Prague, Czech Republic
  • 13University of Manchester, United Kingdom
  • 14Department of Physics, Faculty of Science, University of Zagreb, Zagreb, Croatia
  • 15University of York, United Kingdom
  • 16University of Santiago de Compostela, Spain
  • 17Universitat Politècnica de Catalunya, Spain
  • 18Universidad de Sevilla, Spain
  • 19INFN Laboratori Nazionali del Sud, Catania, Italy
  • 20Istituto nazionale di Astrofisica - Osservatorio Astronomico d'Abruzzo, Italy
  • 21Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, Italy
  • 22Dipartimento di Fisica, Università degli Studi di Bari, Italy
  • 23Instituto de Física Corpuscular, CSIC-Universidad de Valencia, Spain
  • 24Paul Scherrer Institut (PSI), Villingen, Switzerland
  • 25Instituto Superior Técnico, Lisbon, Portugal
  • 26Centro Nacional de Aceleradores (UniversidadSevilla, J. Andalucía, CSIC), Avda Tomas A Edison, 7, 41092 Sevilla, Spain
  • 27Departamento de FAMN, Univsidad Sevilla. Apartado 1065, 41012 Sevilla, Spain
  • 28Joint Institute for Nuclear Research (JINR), Dubna, Russia
  • 29Goethe University Frankfurt, Germany
  • 30Horia Hulubei National Institute of Physics and Nuclear Engineering, Romania
  • 31Japan Atomic Energy Agency (JAEA), Tokai-mura, Japan
  • 32Karlsruhe Institute of Technology, Campus North, IKP, 76021 Karlsruhe, Germany
  • 33National Technical University of Athens, Greece
  • 34Agenzia Nazionale per le Nuove Tecnologie (ENEA), Bologna, Italy
  • 35Physikalisch-Technische Bundesanstalt (PTB), Bundesallee 100, 38116 Braunschweig, Germany
  • 36Istituto Nazionale di Fisica Nucleare, Sezione di Legnaro, Italy
  • 37Consiglio Nazionale delle Ricerche, Bari, Italy
  • 38Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Italy
  • 39Dipartimento di Fisica e Astronomia, Università di Catania, Italy
  • 40University of Ioannina, Greece
  • 41University of Vienna, Faculty of Physics, Vienna, Austria
  • 42University of Granada, Spain
  • 43Department of Physics, University of Basel, Switzerland
  • 44Centre for Astrophysics Research, University of Hertfordshire, United Kingdom
  • 45Bhabha Atomic Research Centre (BARC), India
  • 46Australian National University, Canberra, Australia

  • *Corresponding author: claudia.lederer-woods@ed.ac.uk
  • †Present address: Central Michigan University, Mt. Pleasant, Michigan 48859, US.
  • ‡Present address: Extreme Light Infrastructure—Nuclear Physics, Horia Hulubei National Institute for R&D in Physics and Nuclear Engineering (IFIN-HH), 077125 Bucharest-Mǎgurele, Romania.
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Phys. Rev. C 104, L032803 – Published 22 September, 2021

DOI: https://doi.org/10.1103/PhysRevC.104.L032803

Abstract

Neutron destruction reactions of the cosmic γ-ray emitter Al26 are of importance to determine the amount of Al26 ejected into our galaxy by supernova explosions and for Al26 production in asymptotic giant branch stars. We performed a new measurement of the Al26(n,α) reaction up to 160-keV neutron energy at the neutron time-of-flight facilities n_TOF at CERN and GELINA at EC-JRC. We provide strengths for ten resonances, six of them for the first time. We use our data to calculate astrophysical reactivities for stellar temperatures up to 0.7 GK. Our results resolve a discrepancy between the two previous direct measurements of this reaction, and indicate higher stellar destruction rates than the most recently recommended reactivity.

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Phys. Rev. C 104, L032803– Published 22 September, 2021
  • Received 6 July 2021
  • Accepted 7 September 2021
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