Europium production: neutron star mergers versus core-collapse supernovae

By F. Matteucci, D. Romano, A. Arcones, Oleg Korobkin, Stephan Rosswog. 2013

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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 sup ernovae. We have tested the effects of several important parameters influencing the pro duction of Eu during the merging of two neutron stars, such as: i) the time scale of coalescenc e, ii) the Eu yields and iii) the range of initial masses for the progenitors of the neutron st ars. 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⊙, and the mass range of progenitors of neutron stars is 9‐50 M⊙; 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⊙ per system and type II supernovae, with progenitors in the range 20‐50 M⊙, produce yields of Eu of the order of 10 −8 ‐10 −9 M⊙; iii) either models with only neutron stars producing Eu or mixed ones can reproduce the observed Eu abundance gradient along the Galactic disc.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4c6f3a6f5b685bbc1539edbef3f2a029de6a5769

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Citations in the corpus

The impact of individual nuclear properties on $r$-process nucleosynthesis (2015, background): “ess enhanced halo stars and is a match to the solar residuals. This suggests that whatever mechanism created these elements must have been operating in a consistent fashion since early galactic times [17, 18, 19, 20]. Core-collapse supernovae t the timescale argument, though the promise of early stu”
THE HISTORY OF R-PROCESS ENRICHMENT IN THE MILKY WAY (2014, background): “These differences should surely be imprinted in the enrichment pattern ofr-process elements and may ultimately identify the dominant production mechanism (Argast et al. 2004; Matteucci et al. 2014).”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, result): “…et al. 2004) disfavored them as dominant source of r-process in the early galaxy, more recent studies are either more optimistic about their role (Matteucci et al. 2014) or actually favor them over supernovae as major production site, see for example the recent hydrodynamical studies of Shen et…”
Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way (2018, methodology): “Throughout this study, we also use the GCE code OMEGA (Côté et al. 2017b) in order to explore different DTD functions for NS-NS mergers (see Section 5.3), and to compare with the results of the GCE code of Matteucci et al. (2014) (see orange lines in Figure 3).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “…chemical evolution have revisited this problem in different models with several r-process sources including NS-mergers, NDWs, and MHD-SNe (e.g., Cescutti & Chiappini 2014; Matteucci et al. 2014; Tsujimoto & Shigeyama 2014a,b; van de Voort et al. 2015, B. Wehmeyer et al., 2015, in preparation).”
The Origin of r-process Elements in the Milky Way (2017, background): “…in C17a (which include our own study) cover a wide range of numerical approaches from one-zone models to cosmological hydrodynamic simulations (Matteucci et al. 2014; Cescutti et al. 2015; Hirai et al. 2015; Ishimaru et al. 2015; Shen et al. 2015; Wehmeyer et al. 2015; Komiya & Shigeyama…”
Galactic r-process enrichment by neutron star mergers in cosmological simulations of a Milky Way-mass galaxy (2014, methodology): “In simple models of galactic chemical enrichment, these observations are difficult to reproduce (e.g. Qian 2000; Argast et al. 2004; Matteucci et al. 2014).”
DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2 (2016, background): “…chemical evolution of r-process elements integrated across the Galactic halo (e.g., Mathews et al. 1992; Ishimaru & Wanajo 1999; Argast et al. 2004; Matteucci et al. 2014; Cescutti et al. 2015), within dwarf spheroidal (dSph) galaxies (Tsujimoto & Shigeyama 2014), or within…”
Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, result): “…double BH binaries and of mixed NS+BH systems expected by binary population synthesis models and we translated 12 This paragraph was added during the reviewing process of the present work, after similar conclusions were reached by Matteucci et al. (2014). the predictions into LIGO II rates.”