Neutron Star Mergers Might Not Be the Only Source of r -process Elements in the Milky Way
Abstract
Probing the origin of r-process elements in the universe represents a multidisciplinary challenge. We review the observational evidence that probes the properties of r-process sites, and address them using galactic chemical evolution simulations, binary population synthesis models, and nucleosynthesis calculations. Our motivation is to define which astrophysical sites have significantly contributed to the total mass of r-process elements present in our Galaxy. We found discrepancies with the neutron star (NS–NS) merger scenario. When we assume that they are the only site, the decreasing trend of [Eu/Fe] at [Fe/H] > -1 in the disk of the Milky Way cannot be reproduced while accounting for the delay-time distribution (DTD) of coalescence times (∝t-1) derived from short gamma-ray bursts (GRBs) and population synthesis models. Steeper DTD functions (∝t-1.5) or power laws combined with a strong burst of mergers before the onset of supernovae (SNe) Ia can reproduce the [Eu/Fe] trend, but this scenario is inconsistent with the similar fraction of short GRBs and SNe Ia occurring in early-type galaxies, and it reduces the probability of detecting GW170817 in an early-type galaxy. One solution is to assume an additional production site of Eu that would be active in the early universe, but would fademore »
- Authors:
-
- Hungarian Academy of Sciences, Budapest (Hungary). Konkoly Observatory, Research Centre for Astronomy and Earth Sciences; Michigan States Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab.; Joint Inst. for Nuclear Astrophysics--Center for the Evolution for the Elements (JINA-CEE). East Lansing, MI (United States); NuGrid Collaboration
- Technische Univ. Darmstadt, Darmstadt (Germany). Inst. für Kernphysik
- Technische Univ. Darmstadt, Darmstadt (Germany). Inst. für Kernphysik; GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt (Germany)
- Max Planck Inst. for Astronomy, Heidelberg (Germany)
- Univ. of Trieste, Trieste (Italy). Astronomy Dept.
- Joint Inst. for Nuclear Astrophysics--Center for the Evolution for the Elements (JINA-CEE). East Lansing, MI (United States); Massachusetts Inst. of Technology, Cambridge, MA (United States). Dept. of Physics and Kavli Inst. for Astrophysics and Space Research
- Joint Inst. for Nuclear Astrophysics--Center for the Evolution for the Elements (JINA-CEE). East Lansing, MI (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States). Center for Theoretical Astrophysics; Univ. of Arizona, Tucson, AZ (United States). Dept. of Astronomy; Univ. of New Mexico, Albuquerque, NM (United States). Dept. of Physics and Astronomy; George Washington Univ. Washington D.C. (United States). NuGrid Collaboration
- Hungarian Academy of Sciences, Budapest (Hungary). Konkoly Observatory, Research Centre for Astronomy and Earth Sciences; Joint Inst. for Nuclear Astrophysics--Center for the Evolution for the Elements (JINA-CEE). East Lansing, MI (United States). Univ. of Hull, Hull (United Kingdom). E.A. Milne Centre for Astrophysics, Dept. of Physics & Mathematics; NuGrid Collaboration
- Polish Academy of Sciences, Warsaw (Poland). Nicolaus Copernicus Astronomical Center
- Univ. of Trieste, Trieste (Italy). Astronomy Dept.; I.N.A.F. Osservatorio Astronomico di Trieste, Trieste (Italy); I.N.F.N. Sezione di Trieste, Trieste (Italy)
- Publication Date:
- Research Org.:
- Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE National Nuclear Security Administration (NNSA), Office of Defense Nuclear Nonproliferation
- OSTI Identifier:
- 1565888
- Report Number(s):
- LA-UR-18-28573
Journal ID: ISSN 1538-4357; TRN: US2000929
- Grant/Contract Number:
- 89233218CNA000001
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 875; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy and Astrophysics; galaxy; abundances; stars; nuclear reactions; nucleosynthesis; binaries
Citation Formats
Côté, Benoit, Eichler, Marius, Arcones, Almudena, Hansen, Camilla J., Simonetti, Paolo, Frebel, Anna, Fryer, Chris L., Pignatari, Marco, Reichert, Moritz, Belczynski, Krzysztof, and Matteucci, Francesca. Neutron Star Mergers Might Not Be the Only Source of r -process Elements in the Milky Way. United States: N. p., 2019.
Web. doi:10.3847/1538-4357/ab10db.
Côté, Benoit, Eichler, Marius, Arcones, Almudena, Hansen, Camilla J., Simonetti, Paolo, Frebel, Anna, Fryer, Chris L., Pignatari, Marco, Reichert, Moritz, Belczynski, Krzysztof, & Matteucci, Francesca. Neutron Star Mergers Might Not Be the Only Source of r -process Elements in the Milky Way. United States. https://doi.org/10.3847/1538-4357/ab10db
Côté, Benoit, Eichler, Marius, Arcones, Almudena, Hansen, Camilla J., Simonetti, Paolo, Frebel, Anna, Fryer, Chris L., Pignatari, Marco, Reichert, Moritz, Belczynski, Krzysztof, and Matteucci, Francesca. Sat .
"Neutron Star Mergers Might Not Be the Only Source of r -process Elements in the Milky Way". United States. https://doi.org/10.3847/1538-4357/ab10db. https://www.osti.gov/servlets/purl/1565888.
@article{osti_1565888,
title = {Neutron Star Mergers Might Not Be the Only Source of r -process Elements in the Milky Way},
author = {Côté, Benoit and Eichler, Marius and Arcones, Almudena and Hansen, Camilla J. and Simonetti, Paolo and Frebel, Anna and Fryer, Chris L. and Pignatari, Marco and Reichert, Moritz and Belczynski, Krzysztof and Matteucci, Francesca},
abstractNote = {Probing the origin of r-process elements in the universe represents a multidisciplinary challenge. We review the observational evidence that probes the properties of r-process sites, and address them using galactic chemical evolution simulations, binary population synthesis models, and nucleosynthesis calculations. Our motivation is to define which astrophysical sites have significantly contributed to the total mass of r-process elements present in our Galaxy. We found discrepancies with the neutron star (NS–NS) merger scenario. When we assume that they are the only site, the decreasing trend of [Eu/Fe] at [Fe/H] > -1 in the disk of the Milky Way cannot be reproduced while accounting for the delay-time distribution (DTD) of coalescence times (∝t-1) derived from short gamma-ray bursts (GRBs) and population synthesis models. Steeper DTD functions (∝t-1.5) or power laws combined with a strong burst of mergers before the onset of supernovae (SNe) Ia can reproduce the [Eu/Fe] trend, but this scenario is inconsistent with the similar fraction of short GRBs and SNe Ia occurring in early-type galaxies, and it reduces the probability of detecting GW170817 in an early-type galaxy. One solution is to assume an additional production site of Eu that would be active in the early universe, but would fade away with increasing metallicity. If this is correct, this additional site could be responsible for roughly 50% of the Eu production in the early universe before the onset of SNe Ia. Rare classes of supernovae could be this additional r-process source, but hydrodynamic simulations still need to ensure the conditions for a robust r-process pattern.},
doi = {10.3847/1538-4357/ab10db},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 875,
place = {United States},
year = {Sat Apr 20 00:00:00 EDT 2019},
month = {Sat Apr 20 00:00:00 EDT 2019}
}
Web of Science
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