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Europium production: neutron star mergers versus core-collapse supernovae [ Erratum: 2015MNRAS.447..326M ]
Matteucci, F.; Romano, D.; Arcones, A.; Korobkin, O.; Rosswog, S.
AA(Dipartimento di Fisica, Sezione di Astronomia, Università di Trieste, Via G.B. Tiepolo 11, I-34143 Trieste, Italy; INAF, Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34143 Trieste, Italy; INFN, Sezione di Trieste, Via A. Valerio 2, I-34127 Trieste, Italy; ), AB(INAF, Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy), AC(Institut für Kernphysik, Technische Universität Darmstadt, Schlossgartenstraße 2, D-64289 Darmstadt, Germany; GSI Helmholtzzentrum fuer Schwerionenforschung GmbH, Planckstr. 1, D-64291 Darmstadt, Germany), AD(The Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden), AE(The Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden)
Monthly Notices of the Royal Astronomical Society, Volume 438, Issue 3, p.2177-2185 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
nuclear reactions, nucleosynthesis, abundances, Galaxy: abundances, Galaxy: evolution
Abstract Copyright:
2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


We have explored the Eu production in the Milky Way by means of a very detailed chemical evolution model. In particular, we have assumed that Eu is formed in merging neutron star (or neutron star-black hole) binaries as well as in Type II supernovae. We have tested the effects of several important parameters influencing the production of Eu during the merging of two neutron stars, such as (i) the time-scale of coalescence, (ii) the Eu yields and (iii) the range of initial masses for the progenitors of the neutron stars. The yields of Eu from Type II supernovae are very uncertain, more than those from coalescing neutron stars, so we have explored several possibilities. We have compared our model results with the observed rate of coalescence of neutron stars, the solar Eu abundance, the [Eu/Fe] versus [Fe/H] relation in the solar vicinity and the [Eu/H] gradient along the Galactic disc. Our main results can be summarized as follows: (i) neutron star mergers can be entirely responsible for the production of Eu in the Galaxy if the coalescence time-scale is no longer than 1 Myr for the bulk of binary systems, the Eu yield is around 3 × 10-7 M&sun; and the mass range of progenitors of neutron stars is 9-50 M&sun;; (ii) both Type II supernovae and merging neutron stars can produce the right amount of Eu if the neutron star mergers produce 2 × 10-7 M&sun; per system and Type II supernovae, with progenitors in the range 20-50 M&sun;, produce yields of Eu of the order of 10-8-10-9 M&sun;; (iii) either models with only neutron stars producing Eu or mixed ones can reproduce the observed Eu abundance gradient along the Galactic disc.

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