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Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star
Arcavi, Iair1,2,3; Howell, D. Andrew1,3; Daniel Kasen4,5,6; LarsBildsten2,3; Griffin Hosseinzadeh1,3; CurtisMcCully1,3; Zheng Chuen Wong1,3; Sarah Rebekah Katz1,3; Avishay Gal-Yam7; Jesper Sollerman8; Francesco Taddia8; Giorgos Leloudas7,9; Christoffer Fremling8; Peter E. Nugent6,10; Assaf Horesh7,11; Kunal Mooley12; Clare Rumsey13; S.Bradley Cenko14,15; Melissa L. Graham6,16; Daniel A. Perley9,17; Ehud Nakar18; Nir J. Shaviv11; OmerBromberg18; Ken J. Shen6; Eran O. Ofek7; Yi Cao16,19; Xiaofeng Wang20; Fang Huang20; Liming Rui20; Tianmeng Zhang21,22; Wenxiong Li20; Zhitong Li20; Zhang JJ(张居甲)23,24; Stefano Valenti25; David Guevel1,3; Benjamin Shappee26; Christopher S. Kochanek27,28; Thomas W.-S. Holoien27,28; Alexei V. Filippenko6,29; Rob Fender12; Anders Nyholm8; Ofer Yaron7; Mansi M. Kasliwal30; Mark Sullivan31; Nadja Blagorodnova30; Richard S. Walters30; Ragnhild Lunnan30; Danny Khazov7; Igor Andreoni32,33,34; Russ R. Laher35; Nick Konidaris26; Przemek Wozniak36; Bue, Brian37
Source PublicationNATURE
2017-11-09
Volume551Issue:7679Pages:210-+
DOI10.1038/nature24030
Contribution Rank第23完成单位
Indexed BySCI ; EI
Abstract

Every supernova so far observed has been considered to be the terminal explosion of a star. Moreover, all supernovae with absorption lines in their spectra show those lines decreasing in velocity over time, as the ejecta expand and thin, revealing slower-moving material that was previously hidden. In addition, every supernova that exhibits the absorption lines of hydrogen has one main light-curve peak, or a plateau in luminosity, lasting approximately 100 days before declining(1). Here we report observations of iPTF14hls, an event that has spectra identical to a hydrogen-rich core-collapse supernova, but characteristics that differ extensively from those of known supernovae. The light curve has at least five peaks and remains bright for more than 600 days; the absorption lines show little to no decrease in velocity; and the radius of the line-forming region is more than an order of magnitude bigger than the radius of the photosphere derived from the continuum emission. These characteristics are consistent with a shell of several tens of solar masses ejected by the progenitor star at supernova-level energies a few hundred days before a terminal explosion. Another possible eruption was recorded at the same position in 1954. Multiple energetic pre-supernova eruptions are expected to occur in stars of 95 to 130 solar masses, which experience the pulsational pair instability(2-5). That model, however, does not account for the continued presence of hydrogen, or the energetics observed here. Another mechanism for the violent ejection of mass in massive stars may be required.

Funding ProjectN/A
Funding OrganizationN/A
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
PublisherNATURE PUBLISHING GROUP
Publication PlaceMACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
ISSN0028-0836
URL查看原文
WOS IDWOS:000414734200043
WOS Research AreaScience & Technology - Other Topics
WOS SubjectMultidisciplinary Sciences
WOS KeywordEXPANDING PHOTOSPHERE METHOD ; PULSATIONAL PAIR-INSTABILITY ; II SUPERNOVAE ; HIGH-REDSHIFT ; LIGHT CURVES ; LOW-RESOLUTION ; SKY SURVEY ; TELESCOPE ; GALAXIES ; SPECTROGRAPH
EI Accession Number5266439
EI Classification Number901Geobase: Related Topics
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/11893
Collection丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
Corresponding AuthorArcavi, Iair
Affiliation1.Las Cumbres Observatory, Goleta; CA; 93117, United States
2.Kavli Institute for Theoretical Physics, University of California, Santa Barbara; CA; 93106, United States
3.Department of Physics, University of California, Santa Barbara; CA; 93106, United States
4.Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley; CA; 94720, United States
5.Department of Physics, University of California, Berkeley; CA; 94720, United States
6.Department of Astronomy, University of California, Berkeley; CA; 94720-3411, United States
7.Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot; 76100, Israel
8.Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm; SE-10691, Sweden
9.Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen; 2100, Denmark
10.Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley; CA; 94720, United States
11.Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem; 91904, Israel
12.Department of Physics, Astrophysics, University of Oxford, Denys Wilkinson Building, Oxford; OX1 3RH, United Kingdom
13.Astrophysics Group, Cavendish Laboratory, 19 J. J. Thomson Avenue, Cambridge; CB3 0HE, United Kingdom
14.Astrophysics Science Division, NASA Goddard Space Flight Center, Code 661, Greenbelt; MA; 20771, United States
15.Joint Space-Science Institute, University of Maryland, College Park, Maryland; 20742, United States+6
16.Department of Astronomy, University of Washington, Box 351580, Seattle; WA; 98195-1580, United States
17.Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool; L3 5RF, United Kingdom
18.Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv, 69978, Israel
19.EScience Institute, University of Washington, Box 351570, Seattle; WA; 98195-1580, United States
20.Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing; 100084, China
21.Key Laboratory of Optical Astronomy, National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing; 100012, China
22.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing; 101408, China
23.Yunnan Observatories, Chinese Academy of Sciences, Kunming; 650011, China
24.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Phoenix Mountain, East District, Kunming, Yunnan; 650216, China
25.Department of Physics, University of California, 1 Shields Avenue, Davis; CA; 95616, United States
26.Carnegie Observatories, 813 Santa Barbara Street, Pasadena; CA; 91101, United States
27.Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus; OH; 43210, United States
28.Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, 191 W. Woodruff Avenue, Columbus; OH; 43210, United States
29.Miller Institute for Basic Research in Science, University of California, Berkeley; CA; 94720, United States
30.Cahill Center for Astrophysics, California Institute of Technology, Pasadena; CA; 91125, United States
31.Department of Physics and Astronomy, University of Southampton, Southampton; SO17 1BJ, United Kingdom
32.Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, VIC; 3122, Australia
33.ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia
34.Australian Astronomical Observatory. PO Box 915, North Ryde; NSW; 1670, Australia
35.Spitzer Science Center, California Institute of Technology, MS 314-6, Pasadena; CA; 91125, United States
36.Space and Atmospheric Sciences Group, Mail Stop D466, Los Alamos National Laboratory, Los Alamos; NM; 87545, United States
37.Jet Propulsion Laboratory, California Institute of Technology, Pasadena; CA; 91109, United States
Recommended Citation
GB/T 7714
Arcavi, Iair,Howell, D. Andrew,Daniel Kasen,et al. Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star[J]. NATURE,2017,551(7679):210-+.
APA Arcavi, Iair.,Howell, D. Andrew.,Daniel Kasen.,LarsBildsten.,Griffin Hosseinzadeh.,...&Bue, Brian.(2017).Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star.NATURE,551(7679),210-+.
MLA Arcavi, Iair,et al."Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star".NATURE 551.7679(2017):210-+.
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