论文标题
3C 279的伽马射线耀斑的变异性和光谱行为
Variability and Spectral Behavior of Gamma-ray Flares of 3C 279
论文作者
论文摘要
3C 279显示从2018年1月到2018年6月的费米 - 拉特γ射线观察的通量变化增加。我们进行了详细的费米 - 拉特分析，以调查2018年3C 279的可变性和光谱行为。在这项工作中，我们在这项工作中分析了γ射线光谱和任何镜头（或者均未发现的镜头）（或者均未弄清楚）。这表明耗散区域不在宽线区域之外，并且能量耗散可能是由于compton的反向散射粉尘圆环红外光子的过程，该结果也与Tolamatti等人中的结果一致。使用灰尘圆环（DT）光子的外部逆康普顿散射来计算宽带光谱分布（SED）。我们发现耀斑衰减时间尺度与通过DT光子的相对论电子的冷却时间一致的事实进一步支持了这一模型。在SED建模期间，发现了电子能量分布（EED）相对较难的频谱，并表明这些电子可能不会因耗散区域发生的冲击而加速。此外，由于磁化比低，还排除了磁重新连接。因此，我们建议从斑点外部注入高能电子并增加耀斑。
3C 279 showed enhanced flux variations in Fermi-LAT γ-ray observations from January to June 2018. We present a detailed Fermi-LAT analysis to investigate the variability and spectral behaviors of 3C 279 during the γ-ray flares in 2018. In this work, we analyzed the γ-ray spectra and found that the spectra in either the flaring or quiescent states do not show any clear breaks (or cutoffs). This indicates that the dissipation region is outside the broad-line region, and the energy dissipation may be due to the inverse Compton process of scattering the dust torus infrared photons, this result is also consistent with that in Tolamatti et al. An external inverse Compton scattering of dusty torus (DT) photons is employed to calculate the broadband spectral energy distribution (SED). This model was further supported by the fact that we found flare decay timescale was consistent with the cooling time of relativistic electrons through DT photons. During the SED modeling, a relatively harder spectrum for the electron energy distribution (EED) is found and suggests these electrons may not be accelerated by the shock that happened in the dissipation region. Besides, the magnetic reconnection is also ruled out due to a low magnetization ratio. Thus, we suggest an injection of higher-energy electrons from outside the blob and raising the flare.
