A very luminous magnetar-powered supernova associated with an ultra-long γ-ray burst
A very luminous magnetar-powered supernova associated with an ultra-long γ-ray burst
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DOI：
10.1038/nature14579
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发表时间：
2015-07
期刊：
影响因子：
64.8
通讯作者：
J. Greiner;P. Mazzali;D. A. Kann;T. Krühler;E. Pian;S. Prentice;F. Olivares E.;A. Rossi;S. Klose;S. Taubenberger;F. Knust;P. Afonso;C. Ashall;J. Bolmer;C. Delvaux;R. Diehl;J. Elliott;R. Filgas;J. Fynbo;J. Graham;A. N. Guelbenzu;S. Kobayashi;G. Leloudas;S. Savaglio;P. Schady;S. Schmidl;T. Schweyer;V. Sudilovsky;M. Tanga;A. Updike;Hendrik van Eerten;K. Varela
中科院分区：
文献类型：
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作者：
J. Greiner;P. Mazzali;D. A. Kann;T. Krühler;E. Pian;S. Prentice;F. Olivares E.;A. Rossi;S. Klose;S. Taubenberger;F. Knust;P. Afonso;C. Ashall;J. Bolmer;C. Delvaux;R. Diehl;J. Elliott;R. Filgas;J. Fynbo;J. Graham;A. N. Guelbenzu;S. Kobayashi;G. Leloudas;S. Savaglio;P. Schady;S. Schmidl;T. Schweyer;V. Sudilovsky;M. Tanga;A. Updike;Hendrik van Eerten;K. Varela
最近有人提出了一类新的超长持续时间（超过10，000秒）γ射线爆发，。它们可能起源于恒星的爆炸，这些恒星的半径比那些产生正常长持续时间γ射线爆发的恒星大得多，或者起源于星星的潮汐破裂。目前还没有明确的超新星与超长持续时间的γ射线爆发联系在一起。在这里，我们报告了一颗超新星（SN 2011kl）与超长持续时间γ射线暴GRB 111209A有关，红移为0.677。这颗超新星的亮度是与长持续时间γ射线爆发相关的Ic型超新星的三倍多，它的光谱也明显不同。连续光谱的斜率类似于超亮超新星的斜率，但进一步向下延伸到静止坐标系紫外线，这意味着金属含量较低。光变曲线的演化比超亮超新星的演化要快得多。这种高亮度和低金属线不透明度的组合无法与典型的IC型超新星相协调，但可以通过强磁化中子星星（磁星）注入额外能量的模型来重现，这也被提出作为超亮超新星的解释。
A new class of ultra-long-duration (more than 10,000 seconds) γ-ray bursts has recently been suggested,,. They may originate in the explosion of stars with much larger radii than those producing normal long-duration γ-ray bursts,or in the tidal disruption of a star. No clear supernova has yet been associated with an ultra-long-duration γ-ray burst. Here we report that a supernova (SN 2011kl) was associated with the ultra-long-duration γ-ray burst GRB 111209A, at a redshiftzof 0.677. This supernova is more than three times more luminous than type Ic supernovae associated with long-duration γ-ray bursts,,, and its spectrum is distinctly different. The slope of the continuum resembles those of super-luminous supernovae,, but extends further down into the rest-frame ultraviolet implying a low metal content. The light curve evolves much more rapidly than those of super-luminous supernovae. This combination of high luminosity and low metal-line opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae.