University of Hertfordshire

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By the same authors

129I and 247Cm in meteorites constrain the last astrophysical source of solar r-process elements

Research output: Contribution to journalArticlepeer-review


  • Benoit Côté
  • Marius Eichler
  • Andrés Yagüe López
  • Nicole Vassh
  • Matthew R. Mumpower
  • Blanka Világos
  • Benjámin Soós
  • A. Arcones
  • Trevor M. Sprouse
  • Rebecca Surman
  • Marco Pignatari
  • Mária K. Peto
  • Benjamin Wehmeyer
  • Thomas Rauscher
  • Maria Lugaro
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Original languageEnglish
Pages (from-to)945-948
Number of pages4
Publication statusPublished - 26 Feb 2021
Externally publishedYes


The composition of the early Solar System can be inferred from meteorites. Many elements heavier than iron were formed by the rapid neutron capture process (r-process), but the astrophysical sources where this occurred remain poorly understood. We demonstrate that the near-identical half-lives (−~15:6 million years) of the radioactive r-process nuclei iodine-129 and curium-247 preserve their ratio, irrespective of the time between production and incorporation into the Solar System. We constrain the last r-process source by comparing the measured meteoritic ratio 129I/247Cm = 438 ± 184 with nucleosynthesis calculations based on neutron star merger and magneto-rotational supernova simulations. Moderately neutron-rich conditions, often found in merger disk ejecta simulations, are most consistent with the meteoritic value. Uncertain nuclear physics data limit our confidence in this conclusion.


Funding Information: B.C., A.Y.L., B.W., M.K.P., and M.L. were supported by the ERC Consolidator Grant (Hungary) funding scheme (project RADIOSTAR, G.A. no. 724560). B.C. and M.L. were supported by the Hungarian Academy of Sciences through the Lend?let project LP2014-17. B.C., M.R.M., and M.P. acknowledge support from the National Science Foundation (NSF, United States) under grant no. PHY-1430152 (JINA Center for the Evolution of the Elements). M.R.M. was supported by the U.S. Department of Energy through the Los Alamos National Laboratory and by the Laboratory Directed Research and Development program of Los Alamos National Laboratory under project no. 20190021DR. Los Alamos National Laboratory is operated by Triad National Security, LLC., for the National Nuclear Security Administration of the U.S. Department of Energy (contract no. 89233218CNA000001). M.E. and A.A. acknowledge support from the European Research Council through ERC starting grant no. 677912 EUROPIUM and Deutsche Forschungsgemeinschaft through SFB 1245. N.V. and R.S. were supported by the Fission In R-process Elements (FIRE) topical collaboration in nuclear theory, funded by the U.S. Department of Energy. A.A. was supported by the Helmholtz Forschungsakademie Hessen f?r FAIR. T.M.S. and R.S. were supported by the U.S. Department of Energy SciDAC collaboration TEAMS (DE-SC0018232). T.M.S. was supported by the Los Alamos National Laboratory Center for Space and Earth Science, which is funded by its Laboratory Directed Research and Development program under project no. 20180475DR. M.P. acknowledges support to NuGrid from STFC through the University of Hull's consolidated grant ST/R000840/1. Publisher Copyright: © 2021 American Association for the Advancement of Science. All rights reserved. Copyright: Copyright 2021 Elsevier B.V., All rights reserved.

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