A superluminous supernova lightened by collisions with pulsational pair-instability shells

被引:12
|
作者
Lin, Weili [1 ,2 ]
Wang, Xiaofeng [1 ,2 ,3 ,4 ]
Yan, Lin [5 ]
Gal-Yam, Avishay [6 ]
Mo, Jun [1 ,2 ]
Brink, Thomas G. G. [7 ]
Filippenko, Alexei V. V. [7 ]
Xiang, Danfeng [1 ,2 ]
Lunnan, Ragnhild [8 ,9 ]
Zheng, Weikang [7 ]
Brown, Peter [10 ,11 ]
Kasliwal, Mansi [12 ]
Fremling, Christoffer [12 ]
Blagorodnova, Nadejda [13 ,14 ,15 ]
Mirzaqulov, Davron [16 ]
Ehgamberdiev, Shuhrat A. A. [16 ,17 ]
Lin, Han [1 ,2 ,18 ,19 ]
Zhang, Kaicheng [1 ,2 ]
Zhang, Jicheng [20 ]
Yan, Shengyu [1 ,2 ]
Zhang, Jujia [18 ,19 ,21 ]
Chen, Zhihao [1 ,2 ]
Deng, Licai [22 ,23 ,24 ]
Wang, Kun [22 ]
Xiao, Lin [25 ,26 ,27 ]
Wang, Lingjun [28 ]
机构
[1] Tsinghua Univ, Phys Dept, Beijing, Peoples R China
[2] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing, Peoples R China
[3] Beijing Acad Sci & Technol, Beijing Planetarium, Beijing, Peoples R China
[4] Chinese Acad Sci, Purple Mt Observ, Nanjing, Peoples R China
[5] CALTECH, Caltech Opt Observ, Pasadena, CA USA
[6] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Rehovot, Israel
[7] Univ Calif Berkeley, Dept Astron, Berkeley, CA USA
[8] Stockholm Univ, Oskar Klein Ctr, AlbaNova, Stockholm, Sweden
[9] Stockholm Univ, Dept Astron, AlbaNova, Stockholm, Sweden
[10] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA
[11] George P & Cynthia Woods Mitchell Inst Fundamental, College Stn, TX USA
[12] CALTECH, Div Phys Math & Astron, Pasadena, CA USA
[13] Univ Barcelona UB, Dept Fis & Quant Astrofis FQA, Barcelona, Spain
[14] Univ Barcelona UB, Inst Ciencies Cosmos ICCUB, Barcelona, Spain
[15] Inst Estudis Espacials Catalunya IEEC, Barcelona, Spain
[16] Uzbek Acad Sci, Ulugh Beg Astron Inst, Tashkent, Uzbekistan
[17] Natl Univ Uzbekistan, Tashkent, Uzbekistan
[18] Chinese Acad Sci, Yunnan Observ, Kunming, Peoples R China
[19] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming, Peoples R China
[20] Beijing Normal Univ, Dept Astron, Beijing, Peoples R China
[21] Chinese Acad Sci, Ctr Astron Mega Sci, Beijing, Peoples R China
[22] China West Normal Univ, Dept Astron, Nanchong, Peoples R China
[23] Chinese Acad Sci, CAS Key Lab Opt Astron, Natl Astron Observ, Beijing, Peoples R China
[24] Univ Chinese Acad Sci, Sch Astron & Space Sci, Beijing, Peoples R China
[25] Hebei Univ, Coll Phys Sci & Technol, Dept Phys, Baoding, Peoples R China
[26] Hebei Univ, Key Lab High precis Computat & Applicat Quantum Fi, Baoding, Peoples R China
[27] Res Ctr Computat Phys Hebei Prov, Baoding, Peoples R China
[28] Chinese Acad Sci, Inst High Energy Phys, Astroparticle Phys, Beijing, Peoples R China
基金
美国国家航空航天局; 中国国家自然科学基金; 欧洲研究理事会;
关键词
LOW-RESOLUTION; MASSIVE STARS; CURVES; SYSTEM;
D O I
10.1038/s41550-023-01957-3
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
引用
收藏
页码:779 / +
页数:20
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