蟹式粒子加速器每小时的峰值
Twelve-hour spikes from the Crab Pevatron
摘要：
目标。蟹状星云在2010年9月18日显示出一个巨大的伽马射线耀斑。为了更深入地了解这种现象的起源，我们分析了在耀斑期间几乎同时收集的INTEGRAL（20-500 keV）和FERMI（0.1-300 GeV）数据。方法.我们将现有的数据分为三个不同的组，对应于前耀斑期间，耀斑，和随后的平静。对于每个周期，我们进行定时和光谱分析，以区分脉冲星和周围星云对伽马射线光度的贡献。结果在硬X射线域中没有检测到脉冲轮廓和光谱特性的显著变化。相比之下，我们确定了三个独立的增强持续约12小时的伽马射线通量，并分开约两天的时间间隔。光谱分析表明，通量增强，限制在1 GeV以下，可以模拟的幂律与高能量指数截止，其中无论是截止能量或模型归一化增加了约5倍，相对于耀斑前的排放。我们还确认伽马射线耀斑不是脉冲的。结论.时间和光谱分析表明，伽玛射线耀斑是由于同步辐射从一个非常紧凑的粒子加速器位于脉冲星风和周围的星云之间的相互作用的区域。这是在宇宙加速器中测量到的最高电子能量。耀斑的光谱特性的相对论移动的发射体和/或更硬的发射电子人口的框架中解释。
英文摘要：
Aims. The Crab nebula displayed a large gamma-ray flare on September 18, 2010. To more closely understand the origin of this phenomenon, we analyze the INTEGRAL (20-500 keV) and FERMI (0.1-300 GeV) data collected almost simultaneously during the flare. Methods. We divide the available data into three different sets, corresponding to the pre-flare period, the flare, and the subsequent quiescence. For each period, we perform timing and spectral analyses to differentiate between the contributions of the pulsar and from the surrounding nebula to the gamma-ray luminosity. Results. No significant variations in the pulse profile and spectral characteristics are detected in the hard X-ray domain. In contrast, we identify three separate enhancements in the gamma-ray flux lasting for about 12 hours and separated by an interval of about two days from each other. The spectral analysis shows that the flux enhancement, confined below ~ 1 GeV, can be modelled by a power-law with a high energy exponential cut-off, where either the cut-off energy or the model normalization increased by a factor of ~ 5 relative to the pre-flare emission. We also confirm that the gamma-ray flare is not pulsed. Conclusions. The timing and spectral analysis indicate that the gamma-ray flare is due to synchrotron emission from a very compact Pevatron located in the region of interaction between the pulsar wind and the surrounding nebula. These are the highest electron energies ever measured in a cosmic accelerator. The spectral properties of the flare are interpreted in the framework of a relativistically moving emitter and/or a harder emitting electron population.
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