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A superluminous supernova lightened by collisions with pulsational pair-instability shells
Lin, Weili1; Wang, Xiaofeng1,2,3; Yan, Lin4; Gal-Yam, Avishay5; Mo, Jun1; Brink, Thomas G.6; Filippenko, Alexei V.6; Xiang, Danfeng1; Lunnan, Ragnhild7; Zheng, Weikang6; Brown, Peter8,9; Kasliwal, Mansi10; Fremling, Christoffer10; Blagorodnova, Nadejda11,12,13; Mirzaqulov, Davron14; Ehgamberdiev, Shuhrat A.14,15; Lin H(林含)1,16,17; Zhang, Kaicheng1; Zhang, Jicheng18; Yan, Shengyu1; Zhang JJ(张居甲)16,17,19; Chen, Zhihao1; Deng, Licai20,21,22; Wang, Kun20; Xiao, Lin23,24,25; Wang, Lingjun26
Source PublicationNATURE ASTRONOMY
2023-05
DOI10.1038/s41550-023-01957-3
Contribution Rank第16完成单位
Indexed BySCI
Abstract

Superluminous supernovae are among the most energetic stellar explosions in the Universe, but their energy sources remain an open question. Here we present long-term observations of one of the closest examples of the hydrogen-poor superluminous supernovae subclass SLSNe-I, supernova SN 2017egm, revealing the most complicated known luminosity evolution of SLSNe-I. Three distinct post-peak bumps were recorded in its light curve collected at about 100-350 days after maximum brightness, challenging current popular power models such as magnetar, fallback accretion, and interaction between ejecta and a circumstellar shell. However, the complex light curve can be well modelled by successive interactions with multiple circumstellar shells with a total mass of about 6.8-7.7 M-circle dot. In this scenario, large energy deposition from interaction-induced reverse shocks results in ionization of neutral oxygen in the supernova ejecta and hence a much lower nebular-phase line ratio of [O i] lambda 6,300/([Ca II] + [O II]) lambda 7,300 (similar to 0.2) compared with that derived for other superluminous and normal stripped-envelope supernovae. The pre-existing multiple shells indicate that the progenitor of SN 2017egm experienced pulsational mass ejections triggered by pair instability within 2 years before explosion, in robust agreement with theoretical predictions for a pre-pulsation helium-core mass of 48-51 M-circle dot.

Funding ProjectSwift ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; Center for Astronomical Mega-Science, CAS ; National Aeronautics and Space Administration ; NASA ; W. M. Keck Foundation ; Heising-Simons Foundation ; University of California Observatories - National Natural Science Foundation of China[12288102] ; University of California Observatories - National Natural Science Foundation of China[12033003] ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Tencent Xplorer Prize ; European Union via ERC[725161] ; ISF GW excellence centre ; GIF grants ; Schwartz/Reisman Collaborative Science Program ; Norman E. Alexander Family Foundation ULTRASAT Data Center Fund ; Minerva and Yeda-Sela ; Miller Institute for Basic Research in Science ; Christopher R. Redlich Fund - European Union (ERC)[CET-3PO] ; Christopher R. Redlich Fund - European Union (ERC)[101042610] ; National Natural Science Foundation of China[12103050] ; Advanced Talents Incubation Program of the Hebei University ; Midwest Universities Comprehensive Strength Promotion project ; National Program on Key Research and Development Project of China[2021YFA0718500]
Funding OrganizationSwift ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; Center for Astronomical Mega-Science, CAS ; National Aeronautics and Space Administration ; NASA ; W. M. Keck Foundation ; Heising-Simons Foundation ; University of California Observatories - National Natural Science Foundation of China[12288102, 12033003] ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Tencent Xplorer Prize ; European Union via ERC[725161] ; ISF GW excellence centre ; GIF grants ; Schwartz/Reisman Collaborative Science Program ; Norman E. Alexander Family Foundation ULTRASAT Data Center Fund ; Minerva and Yeda-Sela ; Miller Institute for Basic Research in Science ; Christopher R. Redlich Fund - European Union (ERC)[CET-3PO, 101042610] ; National Natural Science Foundation of China[12103050] ; Advanced Talents Incubation Program of the Hebei University ; Midwest Universities Comprehensive Strength Promotion project ; National Program on Key Research and Development Project of China[2021YFA0718500]
Language英语
Subject Area天文学 ; 恒星与银河系
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle; Early Access
PublisherNATURE PORTFOLIO
Publication PlaceHEIDELBERGER PLATZ 3, BERLIN, 14197, GERMANY
ISSN2397-3366
URL查看原文
WOS IDWOS:000979984200002
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordLOW-RESOLUTION ; MASSIVE STARS ; CURVES ; SYSTEM
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/26023
Collection南方基地
中国科学院天体结构与演化重点实验室
Corresponding AuthorWang, Xiaofeng
Affiliation1.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China;
2.Beijing Planetarium, Beijing Academy of Science and Technology, Beijing, China;
3.Purple Mountain Observatory, Chinese Academy of Science, Nanjing, China;
4.Caltech Optical Observatories, California Institute of Technology, Pasadena, USA;
5.Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel;
6.Department of Astronomy, University of California Berkeley, Berkeley, USA;
7.The Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden;
8.Department of Physics and Astronomy, Texas A&M University, College Station, USA;
9.George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, College Station, USA;
10.Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, USA;
11.Departament de Física Quántica i Astrofísica (FQA), Universitat de Barcelona (UB), Barcelona, Spain;
12.Institut de Ciéncies del Cosmos (ICCUB), Universitat de Barcelona (UB), Barcelona, Spain;
13.Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain;
14.Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Tashkent, Uzbekistan;
15.National University of Uzbekistan, Tashkent, Uzbekistan;
16.Yunnan Observatories, Chinese Academy of Sciences, Kunming, China;
17.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China;
18.Department of Astronomy, Beijing Normal University, Beijing, China;
19.Center for Astronomical Mega-Science, Chinese Academy of Sciences, Chaoyang District, China;
20.Department of Astronomy, China West Normal University, Nanchong, China;
21.CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China;
22.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China;
23.Department of Physics, College of Physical Sciences and Technology, Hebei University, Baoding, China;
24.Key Laboratory of High-precision Computation and Application of Quantum Field Theory of Hebei Province, Hebei University, Baoding, China;
25.Research Center for Computational Physics of Hebei Province, Baoding, China;
26.Astroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, China
Recommended Citation
GB/T 7714
Lin, Weili,Wang, Xiaofeng,Yan, Lin,et al. A superluminous supernova lightened by collisions with pulsational pair-instability shells[J]. NATURE ASTRONOMY,2023.
APA Lin, Weili.,Wang, Xiaofeng.,Yan, Lin.,Gal-Yam, Avishay.,Mo, Jun.,...&Wang, Lingjun.(2023).A superluminous supernova lightened by collisions with pulsational pair-instability shells.NATURE ASTRONOMY.
MLA Lin, Weili,et al."A superluminous supernova lightened by collisions with pulsational pair-instability shells".NATURE ASTRONOMY (2023).
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