Pulsational Pair-instability Supernovae. I. Pre-collapse Evolution and Pulsational Mass Ejection

Abstract

We calculate the evolution of massive stars, which undergo pulsational pair-instability (PPI) when the O-rich core is formed. The evolution from the main-sequence through the onset of PPI is calculated for stars with the initial masses of $80-140$ $M_{\odot }$ and metallicities of $Z=10^{-3}-1.0$ $Z_{\odot }$. Because of mass loss, $Z\le 0.5$ $Z_{\odot }$ is necessary for stars to form He cores massive enough (i.e., mass $>40M_{\odot }$) to undergo PPI. The hydrodynamical phase of evolution from PPI through the beginning of Fe core collapse is calculated for the He cores with masses of $40-62M_{\odot }$ and $Z=0$. During PPI, electron-positron pair production causes a rapid contraction of the O-rich core which triggers explosive O-burning and a pulsation of the core. We study the mass dependence of the pulsation dynamics, thermodynamics, and nucleosynthesis. The pulsations are stronger for more massive He cores and result in such a large amount of mass ejection such as $3-13$ $M_{\odot }$ for $40-62M_{\odot }$ He cores. These He cores eventually undergo Fe-core collapse. The $64M_{\odot }$ He core undergoes complete disruption and becomes a pair-instability supernova. The H-free circumstellar matter ejected around these He cores is massive enough for to explain the observed light curve of Type I (H-free) superluminous supernovae with circumstellar interaction. We also note that the mass ejection sets the maximum mass of black holes (BHs) to be $\sim 50$ $M_{\odot }$, which is consistent with the masses of BHs recently detected by VIRGO and aLIGO.

33 pages, 57 figures, submitted at 29 January 2019, revised at 16 October 2019, accepted at 20 October 2019; published 11 December 2019. References and metadata updated

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