Pulsational Pair-instability Supernovae. I. Pre-collapse Evolution and Pulsational Mass Ejection
Jan 30, 2019
33 pages
Published in:
- Astrophys.J. 887 (2019) 72
e-Print:
- 1901.11136 [astro-ph.HE]
DOI:
- 10.3847/1538-4357/ab4fe5 (publication)
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Abstract: (arXiv)
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 and metallicities of . Because of mass loss, is necessary for stars to form He cores massive enough (i.e., mass ) 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 and . 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 for He cores. These He cores eventually undergo Fe-core collapse. The 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 , which is consistent with the masses of BHs recently detected by VIRGO and aLIGO.Note:
- 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
- electron: pair production
- mass: ejection
- black hole: mass
- star: massive
- supernova
- mass dependence
- thermodynamics
- hydrodynamics
- collapse
References(52)
Figures(61)