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

P. Neyskens, S. Van Eck (), A. Jorissen, S. Goriely, L. Siess and B. Plez
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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

Nature, 2015, vol. 517, issue 7533, 174-176

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.

Date: 2015
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DOI: 10.1038/nature14050

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