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

Leung, Shing-Chi and Nomoto, Ken’ichi and Blinnikov, Sergei (2019) Pulsational Pair-instability Supernovae. I. Pre-collapse Evolution and Pulsational Mass Ejection. Astrophysical Journal, 887 (1). Art. No. 72. ISSN 1538-4357. doi:10.3847/1538-4357/ab4fe5.

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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 initial masses of 80–140 M_⊙ and metallicities of Z = 10⁻³−1.0 Z_⊙. Because of mass loss, Z ≤ 0.5 Z_⊙ is necessary for stars to form He cores massive enough (i.e., mass >40 M_⊙) to undergo PPI. The hydrodynamical phase of evolution from PPI through the beginning of Fe-core collapse is calculated for He cores with masses of 40−62 M_ ⊙ 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 a large amount of mass ejection such as 3–13 M_⊙ for 40−62 M_⊙ He cores. These He cores eventually undergo Fe-core collapse. The 64 M_⊙ He core undergoes complete disruption and becomes a pair-instability supernova. The H-free circumstellar matter ejected around these He cores is massive enough 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 ~50 M_⊙, which is consistent with the masses of BHs recently detected by VIRGO and aLIGO.

Item Type:Article
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URLURL TypeDescription Paper
Leung, Shing-Chi0000-0002-4972-3803
Nomoto, Ken’ichi0000-0001-9553-0685
Blinnikov, Sergei0000-0002-5726-538X
Additional Information:© 2019. The American Astronomical Society. Received 2019 January 29; revised 2019 October 16; accepted 2019 October 20; published 2019 December 11. This work has been supported by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI grant No. JP17K05382. S.B.'s work on PPISNe is supported by the Russian Science Foundation Grant 19-12-00229. We thank the developers of the stellar evolution code MESA for making the code open-source. We also thank Raphael Hirschi for insightful discussion on the stellar evolution of PPISNe and his critical comments. We finally thank Ming-Chung Chu for his assistance in editing the manuscript. Software: MESA (v8118; Paxton et al. 2011, 2013, 2015, 2017).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17K05382
Russian Science Foundation19-12-00229
Subject Keywords:Black holes ; Massive stars ; Stellar mass loss ; Circumstellar matter
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Black holes (162); Massive stars (732); Stellar mass loss (1613); Circumstellar matter (240)
Record Number:CaltechAUTHORS:20191212-145251910
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Official Citation:Shing-Chi Leung et al 2019 ApJ 887 72
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:100281
Deposited By: George Porter
Deposited On:16 Dec 2019 15:28
Last Modified:16 Nov 2021 17:52

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