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Enrichment of Heavy Elements in Chemo-Dynamical Simulations of Dwarf Galaxies

  • Yutaka Hirai (a1), Takayuki R. Saitoh (a2), Shinya Wanajo (a3) (a4) and Michiko S. Fujii (a5)

Abstract

Abundances of heavy elements in dwarf galaxies reflect their early evolutionary histories. Recent astronomical observations have shown that there are star-to-star scatters in the abundances of r-process elements and the decreasing trend of Zn toward higher metallicity in extremely metal-poor stars. However, the enrichment of heavy elements is not well understood. Here we performed a series of high-resolution N-body/smoothed particle hydrodynamics simulations of dwarf galaxies. We find that neutron star mergers can explain ratios of r-process elements to iron in dwarf galaxies due to their suppressed star formation rates. We also find that stars with [Zn/Fe] ≳ 0.5 reflect the ejecta from electron-capture supernovae. Inhomogeneity of the metals in the interstellar medium causes the scatters of heavy elements. We estimate that the timescale of metal mixing is ≲ 40 Myr using heavy element abundances in metal-poor stars.

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Keywords

Enrichment of Heavy Elements in Chemo-Dynamical Simulations of Dwarf Galaxies

  • Yutaka Hirai (a1), Takayuki R. Saitoh (a2), Shinya Wanajo (a3) (a4) and Michiko S. Fujii (a5)

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