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Cobalt-56 γ-ray emission lines from the type Ia supernova 2014J

机译：Ia型超新星2014J的钴56γ射线发射线

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作为宇宙学"标准烛光"的Ia-型超新星被认为来自白矮星的热核爆炸, 同时伴随着大量放射性元素"镍-56"(衰变成钻和铁）的释放。这篇论文报告了对来自一个Ia-型超新星"SN2014J"的"钴-56"γ-射线发射线的首次检测。所观测到的光谱与大到足以对引力坍缩不稳定的一次白矮星爆炸的经典模型大体上一致, 但也不排除存在更复杂的合并情景。%A type Ia supernova is thought to be a thermonuclear explosion of either a single carbon-oxygen white dwarf or a pair of merging white dwarfs. The explosion fuses a large amount of radioactive ~(56)Ni (refs 1-3). After the explosion, the decay chain from ~(56)Ni to ~(56)Co to ~(56)Fe generates γ-ray photons, which are reprocessed in the expanding ejecta and give rise to powerful optical emission. Here we report the detection of ~(56)Co lines at energies of 847 and 1, 238 kiloelectron-volts and a γ-ray continuum in the 200-400 kiloelectronvolt band from the type Ia supernova 2014J in the nearby galaxy M82. The line fluxes suggest that about 0.6 ± 0.1 solar masses of radioactive ~(56)Ni were synthesized during the explosion. The line broadening gives a characteristic mass-weighted ejecta expansion velocity of 10, 000 ± 3, 000 kilometres per second. The observed γ-ray properties are in broad agreement with the canonical model of an explosion of a white dwarf just massive enough to be unstable to gravitational collapse, but do not exclude merger scenarios that fuse comparable amounts of ~(56)Ni.
机译：作为宇宙学"标准烛光"的Ia-型超新星被认为来自白矮星的热核爆炸, 同时伴随着大量放射性元素"镍-56"(衰变成钻和铁）的释放。这篇论文报告了对来自一个Ia-型超新星"SN2014J"的"钴-56"γ-射线发射线的首次检测。所观测到的光谱与大到足以对引力坍缩不稳定的一次白矮星爆炸的经典模型大体上一致, 但也不排除存在更复杂的合并情景。%A type Ia supernova is thought to be a thermonuclear explosion of either a single carbon-oxygen white dwarf or a pair of merging white dwarfs. The explosion fuses a large amount of radioactive ~(56)Ni (refs 1-3). After the explosion, the decay chain from ~(56)Ni to ~(56)Co to ~(56)Fe generates γ-ray photons, which are reprocessed in the expanding ejecta and give rise to powerful optical emission. Here we report the detection of ~(56)Co lines at energies of 847 and 1, 238 kiloelectron-volts and a γ-ray continuum in the 200-400 kiloelectronvolt band from the type Ia supernova 2014J in the nearby galaxy M82. The line fluxes suggest that about 0.6 ± 0.1 solar masses of radioactive ~(56)Ni were synthesized during the explosion. The line broadening gives a characteristic mass-weighted ejecta expansion velocity of 10, 000 ± 3, 000 kilometres per second. The observed γ-ray properties are in broad agreement with the canonical model of an explosion of a white dwarf just massive enough to be unstable to gravitational collapse, but do not exclude merger scenarios that fuse comparable amounts of ~(56)Ni.

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  • 来源
    《Nature》 |2014年第7515期|406-408337|共4页
  • 作者

    E. Churazov; R. Sunyaev; J. Isern; J. Knoedlseder; P. Jean; F. Lebrun; N. Chugai; S. Grebenev; E. Bravo; S. Sazonov; M. Renaud;

  • 作者单位

    Space Research Institute (IKI), Profsouznaya 84/32, Moscow 117997, Russia, Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany;

    Space Research Institute (IKI), Profsouznaya 84/32, Moscow 117997, Russia, Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany;

    Institute for Space Sciences (ICE-CSIC/IEEC), 08193 Bellaterra, Spain;

    Universite de Toulouse, UPS-OMP, IRAP, Toulouse, France, CNRS, IRAP, 9 Avenuecolonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France;

    Universite de Toulouse, UPS-OMP, IRAP, Toulouse, France, CNRS, IRAP, 9 Avenuecolonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France;

    APC, Universite Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cite, 75205 Paris Cedex 13, France;

    Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Street, 119017 Moscow, Russia;

    Space Research Institute (IKI), Profsouznaya 84/32, Moscow 117997, Russia;

    ETSAV, Universitat Politecnica de Catalunya, Carrer Pere Serra 1-15, 08173 Sant Cugat del Valles, Spain;

    Space Research Institute (IKI), Profsouznaya 84/32, Moscow 117997, Russia, Moscow Institute of Physics and Technology, Institutsky pereulok 9, 141700 Dolgoprudny, Russia;

    LUPM, Universite Montpellier 2, CNRS/IN2P3, CC 72, Place Eugene Bataillon, F-34095 Montpellier Cedex 5, France;

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