Electron Capture Supernovae of Super-AGB Stars: Sensitivity on Input Physics

Abstract

Stars of $\sim$ 8 - 10 $M_{\odot }$ on the main-sequence form strongly electron-degenerate O+Ne+Mg core and become super-AGB stars. If such an O+Ne+Mg core grows to 1.38 $M_{\odot }$, electron captures on ${}^{20}$Ne$(e,{\nu }_e{)}^{20}$F$(e,{\nu }_e{)}^{20}$O take place and ignite O-Ne deflagration around the center. In this paper, we perform two-dimensional hydrodynamics simulations of the propagation of the O-Ne flame to see whether such a flame induces a collapse of the O+Ne+Mg core due to subsequent electron capture behind the flame or triggers a thermonuclear explosion. We present a series of models to explore how the outcome depends on model parameters for the central density in the range from $10^{9.80}$ to $10^{10.20}$ g cm${}^{-3}$, flame structure of both centered and off-centered ignition kernels, special and general relativistic effects, turbulent flame speed formula and the treatments of laminar burning phase. We find that the O+Ne+Mg core obtained from stellar evolutionary models has a high tendency to collapse into a neutron star. We obtain the bifurcation between the electron-capture collapse and thermonuclear explosion. We discuss the implication in nucleosynthesis and the possible observational signals of this class of supernovae.

31 pages, 60 figures, submitted to Astrophysical Journal at 30 January 2019, accepted at 26 November 2019, published at 22 January 2020. Text, figures and references updated to match with accepted version. Metadata updated

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