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Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star.
Arcavi, Iair; Howell, D Andrew; Kasen, Daniel; Bildsten, Lars; Hosseinzadeh, Griffin; McCully, Curtis; Wong, Zheng Chuen; Katz, Sarah Rebekah; Gal-Yam, Avishay; Sollerman, Jesper; Taddia, Francesco; Leloudas, Giorgos; Fremling, Christoffer; Nugent, Peter E; Horesh, Assaf; Mooley, Kunal; Rumsey, Clare; Cenko, S Bradley; Graham, Melissa L; Perley, Daniel A; Nakar, Ehud; Shaviv, Nir J; Bromberg, Omer; Shen, Ken J; Ofek, Eran O; Cao, Yi; Wang, Xiaofeng; Huang, Fang; Rui, Liming; Zhang, Tianmeng; Li, Wenxiong; Li, Zhitong; Zhang, Jujia; Valenti, Stefano; Guevel, David; Shappee, Benjamin; Kochanek, Christopher S; Holoien, Thomas W-S; Filippenko, Alexei V; Fender, Rob; Nyholm, Anders; Yaron, Ofer; Kasliwal, Mansi M; Sullivan, Mark; Blagorodnova, Nadja; Walters, Richard S; Lunnan, Ragnhild; Khazov, Danny; Andreoni, Igor; Laher, Russ R.
Afiliação
  • Arcavi I; Las Cumbres Observatory, Goleta, California 93117, USA.
  • Howell DA; Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA.
  • Kasen D; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • Bildsten L; Las Cumbres Observatory, Goleta, California 93117, USA.
  • Hosseinzadeh G; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • McCully C; Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA.
  • Wong ZC; Department of Physics, University of California, Berkeley, California 94720, USA.
  • Katz SR; Department of Astronomy, University of California, Berkeley, California 94720-3411, USA.
  • Gal-Yam A; Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA.
  • Sollerman J; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • Taddia F; Las Cumbres Observatory, Goleta, California 93117, USA.
  • Leloudas G; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • Fremling C; Las Cumbres Observatory, Goleta, California 93117, USA.
  • Nugent PE; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • Horesh A; Las Cumbres Observatory, Goleta, California 93117, USA.
  • Mooley K; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • Rumsey C; Las Cumbres Observatory, Goleta, California 93117, USA.
  • Cenko SB; Department of Physics, University of California, Santa Barbara, California 93106, USA.
  • Graham ML; Department of Particle Physics and Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel.
  • Perley DA; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden.
  • Nakar E; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden.
  • Shaviv NJ; Department of Particle Physics and Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel.
  • Bromberg O; Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100 Copenhagen, Denmark.
  • Shen KJ; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden.
  • Ofek EO; Department of Astronomy, University of California, Berkeley, California 94720-3411, USA.
  • Cao Y; Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA.
  • Wang X; Department of Particle Physics and Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel.
  • Huang F; Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel.
  • Rui L; Department of Physics, Astrophysics, University of Oxford, Denys Wilkinson Building, Oxford OX1 3RH, UK.
  • Zhang T; Astrophysics Group, Cavendish Laboratory, 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK.
  • Li W; Astrophysics Science Division, NASA Goddard Space Flight Center, Code 661, Greenbelt, Maryland 20771, USA.
  • Li Z; Joint Space-Science Institute, University of Maryland, College Park, Maryland 20742, USA.
  • Zhang J; Department of Astronomy, University of California, Berkeley, California 94720-3411, USA.
  • Valenti S; Department of Astronomy, University of Washington, Box 351580, Seattle, Washington 98195-1580, USA.
  • Guevel D; Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100 Copenhagen, Denmark.
  • Shappee B; Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK.
  • Kochanek CS; The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel.
  • Holoien TW; Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel.
  • Filippenko AV; The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel.
  • Fender R; Department of Astronomy, University of California, Berkeley, California 94720-3411, USA.
  • Nyholm A; Department of Particle Physics and Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel.
  • Yaron O; Department of Astronomy, University of Washington, Box 351580, Seattle, Washington 98195-1580, USA.
  • Kasliwal MM; eScience Institute, University of Washington, Box 351570, Seattle, Washington 98195-1580, USA.
  • Sullivan M; Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China.
  • Blagorodnova N; Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China.
  • Walters RS; Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China.
  • Lunnan R; Key Laboratory of Optical Astronomy, National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing 100012, China.
  • Khazov D; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, China.
  • Andreoni I; Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China.
  • Laher RR; Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China.
Nature ; 551(7679): 210-213, 2017 11 08.
Article em En | MEDLINE | ID: mdl-29120417
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. 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. 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.
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Tipo de estudo: Prognostic_studies Idioma: En Revista: Nature Ano de publicação: 2017 Tipo de documento: Article País de afiliação: Estados Unidos
Texto completo
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XML
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Tipo de estudo: Prognostic_studies Idioma: En Revista: Nature Ano de publicação: 2017 Tipo de documento: Article País de afiliação: Estados Unidos