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  • 1
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    A faint type of supernova from a white dwarf with a helium-rich companion (2010)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2010-05-21
    Description: Supernovae are thought to arise from two different physical processes. The cores of massive, short-lived stars undergo gravitational core collapse and typically eject a few solar masses during their explosion. These are thought to appear as type Ib/c and type II supernovae, and are associated with young stellar populations. In contrast, the thermonuclear detonation of a carbon-oxygen white dwarf, whose mass approaches the Chandrasekhar limit, is thought to produce type Ia supernovae. Such supernovae are observed in both young and old stellar environments. Here we report a faint type Ib supernova, SN 2005E, in the halo of the nearby isolated galaxy, NGC 1032. The 'old' environment near the supernova location, and the very low derived ejected mass ( approximately 0.3 solar masses), argue strongly against a core-collapse origin. Spectroscopic observations and analysis reveal high ejecta velocities, dominated by helium-burning products, probably excluding this as a subluminous or a regular type Ia supernova. We conclude that it arises from a low-mass, old progenitor, likely to have been a helium-accreting white dwarf in a binary. The ejecta contain more calcium than observed in other types of supernovae and probably large amounts of radioactive (44)Ti.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Perets, H B -- Gal-Yam, A -- Mazzali, P A -- Arnett, D -- Kagan, D -- Filippenko, A V -- Li, W -- Arcavi, I -- Cenko, S B -- Fox, D B -- Leonard, D C -- Moon, D-S -- Sand, D J -- Soderberg, A M -- Anderson, J P -- James, P A -- Foley, R J -- Ganeshalingam, M -- Ofek, E O -- Bildsten, L -- Nelemans, G -- Shen, K J -- Weinberg, N N -- Metzger, B D -- Piro, A L -- Quataert, E -- Kiewe, M -- Poznanski, D -- England -- Nature. 2010 May 20;465(7296):322-5. doi: 10.1038/nature09056.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel. hperets@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20485429" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 2
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    Supernova 2007bi as a pair-instability explosion (2009)
    Nature Publishing Group (NPG)
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    Publication Date: 2009-12-04
    Description: Stars with initial masses such that 10M[symbol: see text] 〈or= M(initial) 〈or= 100M[symbol: see text], where M[symbol: see text] is the solar mass, fuse progressively heavier elements in their centres, until the core is inert iron. The core then gravitationally collapses to a neutron star or a black hole, leading to an explosion-an iron-core-collapse supernova. By contrast, extremely massive stars with M(initial) 〉or= 140M[symbol: see text] (if such exist) develop oxygen cores with masses, M(core), that exceed 50M[symbol: see text], where high temperatures are reached at relatively low densities. Conversion of energetic, pressure-supporting photons into electron-positron pairs occurs before oxygen ignition and leads to a violent contraction which triggers a nuclear explosion that unbinds the star in a pair-instability supernova. Transitional objects with 100M[symbol: see text] 〈 M(initial) 〈 140M[symbol: see text] may end up as iron-core-collapse supernovae following violent mass ejections, perhaps as a result of brief episodes of pair instability, and may already have been identified. Here we report observations of supernova SN 2007bi, a luminous, slowly evolving object located within a dwarf galaxy. We estimate the exploding core mass to be M(core) approximately 100M[symbol: see text], in which case theory unambiguously predicts a pair-instability supernova. We show that 〉3M[symbol: see text] of radioactive (56)Ni was synthesized during the explosion and that our observations are well fitted by models of pair-instability supernovae. This indicates that nearby dwarf galaxies probably host extremely massive stars, above the apparent Galactic stellar mass limit, which perhaps result from processes similar to those that created the first stars in the Universe.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gal-Yam, A -- Mazzali, P -- Ofek, E O -- Nugent, P E -- Kulkarni, S R -- Kasliwal, M M -- Quimby, R M -- Filippenko, A V -- Cenko, S B -- Chornock, R -- Waldman, R -- Kasen, D -- Sullivan, M -- Beshore, E C -- Drake, A J -- Thomas, R C -- Bloom, J S -- Poznanski, D -- Miller, A A -- Foley, R J -- Silverman, J M -- Arcavi, I -- Ellis, R S -- Deng, J -- England -- Nature. 2009 Dec 3;462(7273):624-7. doi: 10.1038/nature08579.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Benoziyo Center for Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel. avishay.gal-yam@weizmann.ac.il〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19956255" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 3
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    No signature of ejecta interaction with a stellar companion in three type Ia supernovae (2015)
    Nature Publishing Group (NPG)
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    Publication Date: 2015-05-23
    Description: Type Ia supernovae are thought to be the result of a thermonuclear runaway in carbon/oxygen white dwarfs, but it is uncertain whether the explosion is triggered by accretion from a non-degenerate companion star or by a merger with another white dwarf. Observations of a supernova immediately following the explosion provide unique information on the distribution of ejected material and the progenitor system. Models predict that the interaction of supernova ejecta with a companion star or circumstellar debris lead to a sudden brightening lasting from hours to days. Here we present data for three supernovae that are likely to be type Ia observed during the Kepler mission with a time resolution of 30 minutes. We find no signatures of the supernova ejecta interacting with nearby companions. The lack of observable interaction signatures is consistent with the idea that these three supernovae resulted from the merger of binary white dwarfs or other compact stars such as helium stars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Olling, Rob P -- Mushotzky, Richard -- Shaya, Edward J -- Rest, Armin -- Garnavich, Peter M -- Tucker, Brad E -- Kasen, Daniel -- Margheim, Steve -- Filippenko, Alexei V -- England -- Nature. 2015 May 21;521(7552):332-5. doi: 10.1038/nature14455.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astronomy Department, University of Maryland, College Park, Maryland 20742-2421, USA. ; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218, USA. ; Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, USA. ; 1] Mt Stromlo Observatory, The Australian National University, via Cotter Road, Weston Creek, Australian Capital Territory 2611, Australia [2] Department of Astronomy, University of California, Berkeley, California 94720-3411, USA. ; 1] Department of Astronomy, University of California, Berkeley, California 94720-3411, USA [2] Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA. ; Gemini Observatory, Southern Operations Center, c/o AURA, Casilla 603, La Serena, Chile. ; Department of Astronomy, University of California, Berkeley, California 94720-3411, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25993963" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
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  • 4
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    Asphericity in supernova explosions from late-time spectroscopy (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-02-02
    Description: Core-collapse supernovae (CC-SNe) are the explosions that announce the death of massive stars. Some CC-SNe are linked to long-duration gamma-ray bursts (GRBs) and are highly aspherical. One important question is to what extent asphericity is common to all CC-SNe. Here we present late-time spectra for a number of CC-SNe from stripped-envelope stars and use them to explore any asphericity generated in the inner part of the exploding star, near the site of collapse. A range of oxygen emission-line profiles is observed, including a high incidence of double-peaked profiles, a distinct signature of an aspherical explosion. Our results suggest that all CC-SNe from stripped-envelope stars are aspherical explosions and that SNe accompanied by GRBs exhibit the highest degree of asphericity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Maeda, Keiichi -- Kawabata, Koji -- Mazzali, Paolo A -- Tanaka, Masaomi -- Valenti, Stefano -- Nomoto, Ken'ichi -- Hattori, Takashi -- Deng, Jinsong -- Pian, Elena -- Taubenberger, Stefan -- Iye, Masanori -- Matheson, Thomas -- Filippenko, Alexei V -- Aoki, Kentaro -- Kosugi, George -- Ohyama, Youichi -- Sasaki, Toshiyuki -- Takata, Tadafumi -- New York, N.Y. -- Science. 2008 Feb 29;319(5867):1220-3. doi: 10.1126/science.1149437. Epub 2008 Jan 31.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, Kashiwa-no-ha 5-1-5, Kashiwa City, Chiba 277-8582, Japan. maeda@ea.c.u-tokyo.ac.jp〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18239091" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 5
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    An unusually fast-evolving supernova (2009)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2009-11-07
    Description: Analyses of supernovae (SNe) have revealed two main types of progenitors: exploding white dwarfs and collapsing massive stars. Here we describe SN 2002bj, which stands out as different from any SN reported to date. Its light curve rose and declined very rapidly, yet reached a peak intrinsic brightness greater than -18 magnitude. A spectrum obtained 7 days after discovery shows the presence of helium and intermediate-mass elements, yet no clear hydrogen or iron-peak elements. The spectrum only barely resembles that of a type Ia SN, with added carbon and helium. Its properties suggest that SN 2002bj may be representative of a class of progenitors that previously has been only hypothesized: a helium detonation on a white dwarf, ejecting a small envelope of material. New surveys should find many such objects, despite their scarcity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Poznanski, Dovi -- Chornock, Ryan -- Nugent, Peter E -- Bloom, Joshua S -- Filippenko, Alexei V -- Ganeshalingam, Mohan -- Leonard, Douglas C -- Li, Weidong -- Thomas, Rollin C -- New York, N.Y. -- Science. 2010 Jan 1;327(5961):58-60. doi: 10.1126/science.1181709. Epub 2009 Nov 5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA. dovi@berkeley.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19892941" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 6
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    PTF 11kx: a type Ia supernova with a symbiotic nova progenitor (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2012-08-28
    Description: There is a consensus that type Ia supernovae (SNe Ia) arise from the thermonuclear explosion of white dwarf stars that accrete matter from a binary companion. However, direct observation of SN Ia progenitors is lacking, and the precise nature of the binary companion remains uncertain. A temporal series of high-resolution optical spectra of the SN Ia PTF 11kx reveals a complex circumstellar environment that provides an unprecedentedly detailed view of the progenitor system. Multiple shells of circumstellar material are detected, and the SN ejecta are seen to interact with circumstellar material starting 59 days after the explosion. These features are best described by a symbiotic nova progenitor, similar to RS Ophiuchi.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Dilday, B -- Howell, D A -- Cenko, S B -- Silverman, J M -- Nugent, P E -- Sullivan, M -- Ben-Ami, S -- Bildsten, L -- Bolte, M -- Endl, M -- Filippenko, A V -- Gnat, O -- Horesh, A -- Hsiao, E -- Kasliwal, M M -- Kirkman, D -- Maguire, K -- Marcy, G W -- Moore, K -- Pan, Y -- Parrent, J T -- Podsiadlowski, P -- Quimby, R M -- Sternberg, A -- Suzuki, N -- Tytler, D R -- Xu, D -- Bloom, J S -- Gal-Yam, A -- Hook, I M -- Kulkarni, S R -- Law, N M -- Ofek, E O -- Polishook, D -- Poznanski, D -- New York, N.Y. -- Science. 2012 Aug 24;337(6097):942-5. doi: 10.1126/science.1219164.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, CA 93117, USA. bdilday@lcogt.net〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22923575" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 7
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    An asymmetric energetic type Ic supernova viewed off-axis, and a link to gamma ray bursts (2005)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2005-05-28
    Description: Type Ic supernovae, the explosions after the core collapse of massive stars that have previously lost their hydrogen and helium envelopes, are particularly interesting because of their link with long-duration gamma ray bursts. Although indications exist that these explosions are aspherical, direct evidence has been missing. Late-time observations of supernova SN 2003jd, a luminous type Ic supernova, provide such evidence. Recent Subaru and Keck spectra reveal double-peaked profiles in the nebular lines of neutral oxygen and magnesium. These profiles are different from those of known type Ic supernovae, with or without a gamma ray burst, and they can be understood if SN 2003jd was an aspherical axisymmetric explosion viewed from near the equatorial plane. If SN 2003jd was associated with a gamma ray burst, we missed the burst because it was pointing away from us.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mazzali, Paolo A -- Kawabata, Koji S -- Maeda, Keiichi -- Nomoto, Ken'ichi -- Filippenko, Alexei V -- Ramirez-Ruiz, Enrico -- Benetti, Stefano -- Pian, Elena -- Deng, Jinsong -- Tominaga, Nozomu -- Ohyama, Youichi -- Iye, Masanori -- Foley, Ryan J -- Matheson, Thomas -- Wang, Lifan -- Gal-Yam, Avishay -- New York, N.Y. -- Science. 2005 May 27;308(5726):1284-7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan. mazzali@ts.astro.it〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15919986" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
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  • 8
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    Supernova SN 2011fe from an exploding carbon-oxygen white dwarf star (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-12-16
    Description: Type Ia supernovae have been used empirically as 'standard candles' to demonstrate the acceleration of the expansion of the Universe even though fundamental details, such as the nature of their progenitor systems and how the stars explode, remain a mystery. There is consensus that a white dwarf star explodes after accreting matter in a binary system, but the secondary body could be anything from a main-sequence star to a red giant, or even another white dwarf. This uncertainty stems from the fact that no recent type Ia supernova has been discovered close enough to Earth to detect the stars before explosion. Here we report early observations of supernova SN 2011fe in the galaxy M101 at a distance from Earth of 6.4 megaparsecs. We find that the exploding star was probably a carbon-oxygen white dwarf, and from the lack of an early shock we conclude that the companion was probably a main-sequence star. Early spectroscopy shows high-velocity oxygen that slows rapidly, on a timescale of hours, and extensive mixing of newly synthesized intermediate-mass elements in the outermost layers of the supernova. A companion paper uses pre-explosion images to rule out luminous red giants and most helium stars as companions to the progenitor.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nugent, Peter E -- Sullivan, Mark -- Cenko, S Bradley -- Thomas, Rollin C -- Kasen, Daniel -- Howell, D Andrew -- Bersier, David -- Bloom, Joshua S -- Kulkarni, S R -- Kandrashoff, Michael T -- Filippenko, Alexei V -- Silverman, Jeffrey M -- Marcy, Geoffrey W -- Howard, Andrew W -- Isaacson, Howard T -- Maguire, Kate -- Suzuki, Nao -- Tarlton, James E -- Pan, Yen-Chen -- Bildsten, Lars -- Fulton, Benjamin J -- Parrent, Jerod T -- Sand, David -- Podsiadlowski, Philipp -- Bianco, Federica B -- Dilday, Benjamin -- Graham, Melissa L -- Lyman, Joe -- James, Phil -- Kasliwal, Mansi M -- Law, Nicholas M -- Quimby, Robert M -- Hook, Isobel M -- Walker, Emma S -- Mazzali, Paolo -- Pian, Elena -- Ofek, Eran O -- Gal-Yam, Avishay -- Poznanski, Dovi -- England -- Nature. 2011 Dec 14;480(7377):344-7. doi: 10.1038/nature10644.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA. penugent@lbl.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22170680" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 9
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    Exclusion of a luminous red giant as a companion star to the progenitor of supernova SN 2011fe (2011)
    Nature Publishing Group (NPG)
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    Publication Date: 2011-12-16
    Description: Type Ia supernovae are thought to result from a thermonuclear explosion of an accreting white dwarf in a binary system, but little is known of the precise nature of the companion star and the physical properties of the progenitor system. There are two classes of models: double-degenerate (involving two white dwarfs in a close binary system) and single-degenerate models. In the latter, the primary white dwarf accretes material from a secondary companion until conditions are such that carbon ignites, at a mass of 1.38 times the mass of the Sun. The type Ia supernova SN 2011fe was recently detected in a nearby galaxy. Here we report an analysis of archival images of the location of SN 2011fe. The luminosity of the progenitor system (especially the companion star) is 10-100 times fainter than previous limits on other type Ia supernova progenitor systems, allowing us to rule out luminous red giants and almost all helium stars as the mass-donating companion to the exploding white dwarf.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Li, Weidong -- Bloom, Joshua S -- Podsiadlowski, Philipp -- Miller, Adam A -- Cenko, S Bradley -- Jha, Saurabh W -- Sullivan, Mark -- Howell, D Andrew -- Nugent, Peter E -- Butler, Nathaniel R -- Ofek, Eran O -- Kasliwal, Mansi M -- Richards, Joseph W -- Stockton, Alan -- Shih, Hsin-Yi -- Bildsten, Lars -- Shara, Michael M -- Bibby, Joanne -- Filippenko, Alexei V -- Ganeshalingam, Mohan -- Silverman, Jeffrey M -- Kulkarni, S R -- Law, Nicholas M -- Poznanski, Dovi -- Quimby, Robert M -- McCully, Curtis -- Patel, Brandon -- Maguire, Kate -- Shen, Ken J -- England -- Nature. 2011 Dec 14;480(7377):348-50. doi: 10.1038/nature10646.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of California, Berkeley, California 94720-3411, USA. weidong@berkeley.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22170681" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
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  • 10
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    An outburst from a massive star 40 days before a supernova explosion (2013)
    Nature Publishing Group (NPG)
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    Publication Date: 2013-02-08
    Description: Some observations suggest that very massive stars experience extreme mass-loss episodes shortly before they explode as supernovae, as do several models. Establishing a causal connection between these mass-loss episodes and the final explosion would provide a novel way to study pre-supernova massive-star evolution. Here we report observations of a mass-loss event detected 40 days before the explosion of the type IIn supernova SN 2010mc (also known as PTF 10tel). Our photometric and spectroscopic data suggest that this event is a result of an energetic outburst, radiating at least 6 x 10(47) erg of energy and releasing about 10(-2) solar masses of material at typical velocities of 2,000 km s(-1). The temporal proximity of the mass-loss outburst and the supernova explosion implies a causal connection between them. Moreover, we find that the outburst luminosity and velocity are consistent with the predictions of the wave-driven pulsation model, and disfavour alternative suggestions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ofek, E O -- Sullivan, M -- Cenko, S B -- Kasliwal, M M -- Gal-Yam, A -- Kulkarni, S R -- Arcavi, I -- Bildsten, L -- Bloom, J S -- Horesh, A -- Howell, D A -- Filippenko, A V -- Laher, R -- Murray, D -- Nakar, E -- Nugent, P E -- Silverman, J M -- Shaviv, N J -- Surace, J -- Yaron, O -- England -- Nature. 2013 Feb 7;494(7435):65-7. doi: 10.1038/nature11877.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Benoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel. eran@astro.caltech.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23389540" target="_blank"〉PubMed〈/a〉
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