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Chemo-dynamical evolution model: Enrichment of r-process elements in the Local Group dwarf galaxies

  • Yutaka Hirai (a1) (a2) (a3), Yuhri Ishimaru (a4) (a5), Takayuki R. Saitoh (a6), Michiko S. Fujii (a2), Jun Hidaka (a2) (a7) and Toshitaka Kajino (a1) (a2)...

Neutron star mergers are one of the candidate astrophysical site(s) of r-process. Several chemical evolution studies however pointed out that the observed abundance of r-process is difficult to reproduce by neutron star mergers. In this study, we aim to clarify the enrichment of r-process elements in the Local Group dwarf galaxies. We carry out numerical simulations of galactic chemo-dynamical evolution using an N-body/smoothed particle hydrodynamics code, ASURA. We construct a chemo-dynamical evolution model for dwarf galaxies assuming that neutron star mergers are the major source of r-process elements. Our models reproduce the observed dispersion in [Eu/Fe] as a function of [Fe/H] with neutron star mergers with a merger time of 100 Myr. We find that star formation efficiency and metal mixing processes during the first ≲ 300 Myr of galaxy evolution are important to reproduce the observations. This study supports that neutron star mergers are a major site of r-process.

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D. Argast , M. Samland , F.-K. Thielemann , & Y.-Z. Qian 2004, A&A, 416, 997

Y. Hirai , Y. Ishimaru , T. R. Saitoh , M. S. Fujii , J. Hidaka , & T. Kajino 2015, ApJ, 814, 41

Y. Ishimaru , S. Wanajo , & N. Prantzos 2015, ApJ, (Letter), 804, L35

Y. Revaz & P. Jablonka 2012, A&A, 538, A82

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Proceedings of the International Astronomical Union
  • ISSN: 1743-9213
  • EISSN: 1743-9221
  • URL: /core/journals/proceedings-of-the-international-astronomical-union
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