Stellar Yields of Rotating Pair Instability Supernovae and Comparison with Observations

Koh Takahashi

doi:10.1007/978-3-030-13876-9_86

Stellar Yields of Rotating Pair Instability Supernovae and Comparison with Observations

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

A very-massive star forming a massive CO core of 60â€“120M is considered to explode as a pair-instability supernova (PISN). We have calculated the PISN nucleosynthesis taking both rotating and non-rotating progenitors for the first time to conduct a systematic comparison between theoretical yields and a large sample of metal-poor star abundances. We have found that the predicted low [Na/Mg] -1.5 and high [Ca/Mg] 0.5â€“1.3 abundance ratios are the most important to discriminate PISN signatures from normal metal-poor star abundances, and have confirmed that no currently observed metal-poor star matches with the PISN abundance. The confirmation of the non-detection may indicate that something important is missing from current understanding of stellar physics. Finally, we discuss that qualitatively different stellar evolution, which is against the PISN explosion, results from a CO core with a higher C fraction than canonical models.

Original language	English
Title of host publication	Nuclei in the Cosmos XV
Editors	Alba Formicola, Matthias Junker, Lucio Gialanella, Gianluca Imbriani
Publisher	Springer Science and Business Media, LLC
Pages	445-448
Number of pages	4
ISBN (Print)	9783030138752
DOIs	https://doi.org/10.1007/978-3-030-13876-9_86
Publication status	Published - 2019
Externally published	Yes
Event	15th International Symposium on Nuclei in the Cosmos, NIC 2018 - L'Aquila, Italy Duration: 2018 Jun 24 → 2018 Jun 29

Publication series

Name	Springer Proceedings in Physics
Volume	219
ISSN (Print)	0930-8989
ISSN (Electronic)	1867-4941

Conference

Conference	15th International Symposium on Nuclei in the Cosmos, NIC 2018
Country/Territory	Italy
City	L'Aquila
Period	18/6/24 → 18/6/29

ASJC Scopus subject areas

Physics and Astronomy(all)

Access to Document

10.1007/978-3-030-13876-9_86

Cite this

Stellar Yields of Rotating Pair Instability Supernovae and Comparison with Observations. / Takahashi, Koh.

Nuclei in the Cosmos XV. ed. / Alba Formicola; Matthias Junker; Lucio Gialanella; Gianluca Imbriani. Springer Science and Business Media, LLC, 2019. p. 445-448 (Springer Proceedings in Physics; Vol. 219).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Takahashi, K 2019, Stellar Yields of Rotating Pair Instability Supernovae and Comparison with Observations. in A Formicola, M Junker, L Gialanella & G Imbriani (eds), Nuclei in the Cosmos XV. Springer Proceedings in Physics, vol. 219, Springer Science and Business Media, LLC, pp. 445-448, 15th International Symposium on Nuclei in the Cosmos, NIC 2018, L'Aquila, Italy, 18/6/24. https://doi.org/10.1007/978-3-030-13876-9_86

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abstract = "A very-massive star forming a massive CO core of 60{\^a}€“120M is considered to explode as a pair-instability supernova (PISN). We have calculated the PISN nucleosynthesis taking both rotating and non-rotating progenitors for the first time to conduct a systematic comparison between theoretical yields and a large sample of metal-poor star abundances. We have found that the predicted low [Na/Mg] -1.5 and high [Ca/Mg] 0.5{\^a}€“1.3 abundance ratios are the most important to discriminate PISN signatures from normal metal-poor star abundances, and have confirmed that no currently observed metal-poor star matches with the PISN abundance. The confirmation of the non-detection may indicate that something important is missing from current understanding of stellar physics. Finally, we discuss that qualitatively different stellar evolution, which is against the PISN explosion, results from a CO core with a higher C fraction than canonical models.",

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