THE HISTORY OF R-PROCESS ENRICHMENT IN THE MILKY WAY

By S. Shen, R. Cooke, E. Ramirez-Ruiz, P. Madau, Lucio Mayer, J. Guedes. 2014

142 citations recorded by the source corpus.

We investigate the production sites and the enrichment history of r-process elements in the Galaxy, as traced by the [Eu/Fe] ratio, using the high resolution, cosmological zoom-in simulation “Eris.” At z = 0, Eris represents a close analog to the Milky Way, making it the ideal laboratory to understand the chemical evolution of our Galaxy. Eris formally traces the production of oxygen and iron due to supernovae (SNe) Ia and SNe II. We include in post-processing the production of r-process elements from compact binary mergers. Unlike previous studies, we find that the nucleosynthetic products from compact binary mergers can be incorporated into stars of very low metallicity and at early times, even with a minimum delay time of 100 Myr. This conclusion is relatively insensitive to modest variations in the merger rate, minimum delay time, and the delay time distribution. By implementing a first-order prescription for metal mixing, we can further improve the agreement between our model and the data for the chemical evolution of both [α/Fe] and [Eu/Fe]. We argue that compact binary mergers could be the dominant source of r-process nucleosynthesis in the Galaxy.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/505928c6465a80e9d89db768cc157a1a6d617b21

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “…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 al. (2015) and van de Voort et al. (2015).”
Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, methodology): “…previous arguments against mergers being dominant r-process sites based on Galactic chemical evolution and the observed prompt enrichment of r-process nuclei in metal poor stars (e.g. Argast et al. 2004) have been challenged (e.g., van de Voort et al. 2015; Shen et al. 2015; Hirai et al. 2015).”
The Combined Ultraviolet, Optical, and Near-infrared Light Curves of the Kilonova Associated with the Binary Neutron Star Merger GW170817: Unified Data Set, Analytic Models, and Physical Implications (2017, result): “…future events is shown to be at the high end of the current estimates, the results inferred here would indicate that a large fraction of synthesized r-process material may remain in the gas phase within the interstellar medium or escape the galaxy entirely via galactic winds (Shen et al. 2015).”
First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium (2017, methodology): “…et al. 2013; Hirschmann et al. 2016; De Lucia et al. 2017) and simulations of individual galaxies (Guedes et al. 2011; van de Voort et al. 2015; Shen et al. 2015; van de Voort et al. 2017) by providing a statistical analysis of how abundance patterns are affected by galaxy formation histories…”
The IllustrisTNG simulations: public data release (2018, methodology): “To obtain physical values in units of solar masses, this ﬁeld must be multiplied by α / α 0 where α is the desired mass ejected per NS-NS merger event, and α 0 is the base value (arbitrary) used in the simulation, e.g. Shen et al. (2015) take α = 0.05M (cid”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “Models of different degrees of sophistication have been developed along those lines, from a simple semianalytic models summing up the different sub-halo chemical histories (Salvadori et al. 2007; Komiya et al. 2014) up to full cosmological simulation (e.g. Shen et al. 2015).”
DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2 (2016, background): “…Argast et al. 2004; Matteucci et al. 2014; Cescutti et al. 2015), within dwarf spheroidal (dSph) galaxies (Tsujimoto & Shigeyama 2014), or within cosmologically-motivated galaxy merger models and simulations (Komiya et al. 2014; Ishimaru et al. 2015; Shen et al. 2015; van de Voort et al. 2015).”
The Origin of r-process Elements in the Milky Way (2017, methodology): “…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 2016, see also van de Voort et al. 2015 and Naiman et al. 2017).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “When neutron stars merge, they not only make r-process elements (Rosswog et al., 2014; Shen et al., 2015), but also gravitational waves that may be detectable in the near future (Agathos et al., 2015, Section 7.4).”
Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, background): “In more recent models of galactic chemical evolution performed within cosmological zoom-in simulations (Shen et al. 2015; van de Voort et al. 2015) or by accounting for accretion of sub-halos into the Milky Way halo (Ishimaru et al. 2015) these problems seem to be mitigated and better agreement…”
Simulating galaxy formation with the IllustrisTNG model (2017, methodology): “Following the method of Shen et al. (2015), we use a power-law delay time distribution (Piran 1992; Kalogera et al. 2001) with the same DTD index (1.12) but with a different cut off time scale and normalization as compared to the SNIa DTD (see Naiman et al. 2017, for more details).”