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The temperature and chronology of heavy-element synthesis in low-mass stars

Author

Listed:
  • P. Neyskens

    (Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles (ULB), CP 226, 1050 Bruxelles, Belgium)

  • S. Van Eck

    (Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles (ULB), CP 226, 1050 Bruxelles, Belgium)

  • A. Jorissen

    (Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles (ULB), CP 226, 1050 Bruxelles, Belgium)

  • S. Goriely

    (Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles (ULB), CP 226, 1050 Bruxelles, Belgium)

  • L. Siess

    (Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles (ULB), CP 226, 1050 Bruxelles, Belgium)

  • B. Plez

    (Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS, F-34095 Montpellier, France)

Abstract

Spectrographically obtained zirconium, niobium and technetium abundances in a sample of low-mass stars of type S are used to determine that, in these stars, heavy elements are synthesized by the slow-neutron-capture process at a temperature of less than about 250 million kelvin, and that the process began one million to three million years ago.

Suggested Citation

  • P. Neyskens & S. Van Eck & A. Jorissen & S. Goriely & L. Siess & B. Plez, 2015. "The temperature and chronology of heavy-element synthesis in low-mass stars," Nature, Nature, vol. 517(7533), pages 174-176, January.
    • Handle: RePEc:nat:nature:v:517:y:2015:i:7533:d:10.1038_nature14050
    DOI: 10.1038/nature14050
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