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Constraining the astrophysical $i$ process: The ${}^{87}{Kr} (n, γ) {}^{88}{Kr}$ reaction rate

S. Uthayakumaar ^1,*, A. Spyrou ^1,2, C. Harris ^1,2, P. A. Denissenkov ^3,4, D. Mücher ⁵, H. C. Berg ^1,2, J. A. Clark ⁶, P. A. DeYoung ⁷, A. C. Dombos ¹ et al.

B. Greaves ⁸, M. Guttormsen ⁹, F. Herwig ^3,4, A. C. Larsen ⁹, S. N. Liddick ^1,10, S. Lyons¹¹, J. Owens-Fryar ^1,2, A. Palmisano-Kyle ¹², G. Perdikakis ¹³, A. L. Richard ^1,14, D. Santiago-Gonzalez ⁶, G. Savard ⁶, S. Siem ⁹, M. K. Smith ¹, W. W. von Seeger ¹⁵, and M. Wiedeking ¹⁶

¹Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
²Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
³Astronomy Research Centre and Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia V8W 2Y2, Canada
⁴NuGrid Collaboration, http://nugridstars.org
⁵Institut für Kernphysik der Universität zu Köln, Zülpicher Strasse 77, D-50937 Köln, Germany
⁶Physics Division, Argonne National Laboratory, Lemont, Illinois 60439, USA
⁷Department of Physics, Hope College, Holland, Michigan 49423, USA
⁸Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
⁹Department of Physics, University of Oslo, NO-0316 Oslo, Norway
¹⁰Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
¹¹Pacific Northwest National Laboratory, Richland, Washington 99354, USA
¹²Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
¹³Department of Physics, Central Michigan University, Mount Pleasant, Michigan 48859, USA
¹⁴Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
¹⁵Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
¹⁶Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA

^*Contact author: uthayaku@frib.msu.edu

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Phys. Rev. C 113, 065801 – Published 1 June, 2026

DOI: https://doi.org/10.1103/x665-sgt7

Abstract

Recent astronomical observations indicate that additional nucleosynthesis pathways are required to understand some atypical elemental abundance patterns revealed by new observations. One such process that can help to explain these observations is the intermediate neutron-capture process ( $i$ process). The nuclear properties of isotopes involved in this nucleosynthesis pathway are experimentally well constrained with the exception of the neutron-capture reaction rates, which are provided almost entirely by theory. In this paper, the first experimentally constrained reaction rate on the ${}^{87}{Kr} (n, γ) {}^{88}{Kr}$ reaction is provided by employing the $β$ -Oslo method. The impact of this reaction on the abundance of rubidium within the $i$ process is investigated.

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Constraining the astrophysical $i$ process: The ${}^{87}{Kr} (n, γ) {}^{88}{Kr}$ reaction rate

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Constraining the astrophysical i process: The Kr87(n,γ)Kr88 reaction rate

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Constraining the astrophysical $i$ process: The ${}^{87}{Kr} (n, γ) {}^{88}{Kr}$ reaction rate