Can Neutron Star Mergers Alone Explain the r-process Enrichment of the Milky Way?

Comparing Galactic chemical evolution models to the observed elemental abundances in the Milky Way, we show that neutron star mergers can be a leading r-process site only if at low metallicities such mergers have very short delay times and significant ejecta masses that are facilitated by the masses...

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Published inAstrophysical journal. Letters Vol. 943; no. 2; p. L12
Main Authors Kobayashi, Chiaki, Mandel, Ilya, Belczynski, Krzysztof, Goriely, Stephane, Janka, Thomas H., Just, Oliver, Ruiter, Ashley J., Vanbeveren, Dany, Kruckow, Matthias U., Briel, Max M., Eldridge, Jan J., Stanway, Elizabeth
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.02.2023
IOP Publishing
Subjects
Abundance
Astronomical models
Binary stars
Black holes
Chemical abundances
Chemical evolution
Compact objects
Delay time
Ejecta
Evolution
Galactic evolution
Galaxy chemical evolution
Milky Way
Milky Way Galaxy
Neutron stars
Nucleosynthesis
R-process
Star mergers
Stars
Supernovae
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Abstract Comparing Galactic chemical evolution models to the observed elemental abundances in the Milky Way, we show that neutron star mergers can be a leading r-process site only if at low metallicities such mergers have very short delay times and significant ejecta masses that are facilitated by the masses of the compact objects. Namely, black hole–neutron star mergers, depending on the black hole spins, can play an important role in the early chemical enrichment of the Milky Way. We also show that none of the binary population synthesis models used in this Letter, i.e., COMPAS, StarTrack, Brussels, ComBinE, and BPASS, can currently reproduce the elemental abundance observations. The predictions are problematic not only for neutron star mergers, but also for Type Ia supernovae, which may point to shortcomings in binary evolution models.
AbstractList Comparing Galactic chemical evolution models to the observed elemental abundances in the Milky Way, we show that neutron star mergers can be a leading r-process site only if at low metallicities such mergers have very short delay times and significant ejecta masses that are facilitated by the masses of the compact objects. Namely, black hole–neutron star mergers, depending on the black hole spins, can play an important role in the early chemical enrichment of the Milky Way. We also show that none of the binary population synthesis models used in this Letter, i.e., COMPAS, StarTrack, Brussels, ComBinE, and BPASS, can currently reproduce the elemental abundance observations. The predictions are problematic not only for neutron star mergers, but also for Type Ia supernovae, which may point to shortcomings in binary evolution models.
Author Mandel, Ilya
Ruiter, Ashley J.
Briel, Max M.
Eldridge, Jan J.
Goriely, Stephane
Janka, Thomas H.
Just, Oliver
Vanbeveren, Dany
Kruckow, Matthias U.
Stanway, Elizabeth
Belczynski, Krzysztof
Kobayashi, Chiaki
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  orcidid: 0000-0002-4343-0487
  surname: Kobayashi
  fullname: Kobayashi, Chiaki
  organization: University of Hertfordshire Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, Hatfield AL10 9AB, UK
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  givenname: Ilya
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  surname: Mandel
  fullname: Mandel, Ilya
  organization: The ARC Centre of Excellence for Gravitational Wave Discovery—OzGrav, Australia
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  givenname: Krzysztof
  surname: Belczynski
  fullname: Belczynski, Krzysztof
  organization: Polish Academy of Sciences Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
– sequence: 4
  givenname: Stephane
  surname: Goriely
  fullname: Goriely, Stephane
  organization: Université Libre de Bruxelles Institut d’Astronomie et d’Astrophysique, CP-226, B-1050 Brussels, Belgium
– sequence: 5
  givenname: Thomas H.
  orcidid: 0000-0002-0831-3330
  surname: Janka
  fullname: Janka, Thomas H.
  organization: Max-Planck-Institut für Astrophysik , Postfach 1317, D-85741 Garching, Germany
– sequence: 6
  givenname: Oliver
  orcidid: 0000-0002-3126-9913
  surname: Just
  fullname: Just, Oliver
  organization: Astrophysical Big Bang Laboratory, RIKEN Cluster for Pioneering Research, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
– sequence: 7
  givenname: Ashley J.
  orcidid: 0000-0002-4794-6835
  surname: Ruiter
  fullname: Ruiter, Ashley J.
  organization: University of New South Wales Canberra School of Science, The Australian Defence Force Academy, Canberra, 2600 ACT, Australia
– sequence: 8
  givenname: Dany
  surname: Vanbeveren
  fullname: Vanbeveren, Dany
  organization: Vrije Universiteit Brussel Department of Physics and Astronomy, Brussels, Belgium
– sequence: 9
  givenname: Matthias U.
  orcidid: 0000-0001-9331-0400
  surname: Kruckow
  fullname: Kruckow, Matthias U.
  organization: Université de Genève Département d’Astronomie, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
– sequence: 10
  givenname: Max M.
  surname: Briel
  fullname: Briel, Max M.
  organization: The University of Auckland Department of Physics, Faculty of Science, Auckland, New Zealand
– sequence: 11
  givenname: Jan J.
  orcidid: 0000-0002-1722-6343
  surname: Eldridge
  fullname: Eldridge, Jan J.
  organization: The University of Auckland Department of Physics, Faculty of Science, Auckland, New Zealand
– sequence: 12
  givenname: Elizabeth
  orcidid: 0000-0002-8770-809X
  surname: Stanway
  fullname: Stanway, Elizabeth
  organization: University of Warwick Department of Physics, Gibbet Hill Road, Coventry CV4 7AL, UK
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SubjectTerms Abundance
Astronomical models
Binary stars
Black holes
Chemical abundances
Chemical evolution
Compact objects
Delay time
Ejecta
Evolution
Galactic evolution
Galaxy chemical evolution
Milky Way
Milky Way Galaxy
Neutron stars
Nucleosynthesis
R-process
Star mergers
Stars
Supernovae
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Title Can Neutron Star Mergers Alone Explain the r-process Enrichment of the Milky Way?
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