Blazars exhibit flares across the electromagnetic spectrum. Many $γ$-ray flares are highly correlated with flares detected at optical wavelengths; however, a small subset appears to occur in isolation, with little or no variability detected at longer wavelengths. These "orphan" $γ$-ray flares challenge current models of blazar variability, most of which are unable to reproduce this type of behavior. We present numerical calculations of the time-variable emission of a blazar based on a proposal by Marscher et al. (2010) to explain such events. In this model, a plasmoid ("blob") propagates relativistically along the spine of a blazar jet and passes through a synchrotron-emitting ring of electrons representing a shocked portion of the jet sheath. This ring supplies a source of seed photons that are inverse-Compton scattered by the electrons in the moving blob. The model includes the effects of radiative cooling, a spatially varying magnetic field, and acceleration of the blob's bulk velocity. Synthetic light curves produced by our model are compared to the observed light curves from an orphan flare that was coincident with the passage of a superluminal knot through the inner jet of the blazar PKS 1510$-$089. In addition, we present Very Long Baseline Array polarimetric observations that point to the existence of a jet sheath in PKS 1510$-$089, thus providing further observational support for the plausibility of our model. An estimate of the bolometric luminosity of the sheath within PKS 1510$-$089 is made, yielding $L_{\rm sh} \sim 3 \times 10^{45} ~ \rm erg ~ \rm s^{-1}$. This indicates that the sheath within PKS 1510$-$089 is potentially a very important source of seed photons.
Role of magnetic reconnection in blazar variability using numerical simulation
Indian Institute of Technology Indore（印度印多尔理工学院）；Max-Planck Institute for Astronomy (MPIA)（马克斯·普朗克天文学研究所）；Institute for Theoretical Physics and Astrophysics, Universität Würzburg（维尔茨堡大学理论与物理天体物理研究所）
Could a plasma in quasi-thermal equilibrium be associated to the "orphan" TeV flares ?
TeV $γ$ -射线探测在耀斑状态下没有活动的X射线从耀变体吸引了很多关注，由于这些“孤儿”耀斑的不规则性。虽然同步加速器自康普顿模型已经非常成功地解释了这些源的光谱能量分布和光谱可变性，它还没有能够描述这些非典型的耀斑事件。另一方面，在AGN喷流底部的电子-正电子对等离子体被认为是相对论外流体加速的机制。这种处于准热平衡的等离子体被称为温火球，它发射出MeV峰值能量的辐射，作为加速质子的目标。在这项工作中，我们描述了“孤儿”TeV耀斑耀变体1 ES 1959+650和Mrk 421假设几何考虑在射流和引起费米加速质子和MeV峰值目标光子来自温火球的相互作用。在成功地描述了这些“孤儿”TeV耀斑后，我们关联了TeV $γ$射线、中微子和UHECR通过p $γ$相互作用的通量，并分别计算了IceCube/AMANDA和TA实验中预期的高能中微子和UHECR的数目.此外，在Wein火球中主要通过电子正电子湮没产生的MeV热中微子也可以通过它传播.通过考虑两个中微子（太阳、大气和加速器参数）和三个中微子的混合，我们研究了共振振荡，估计了中微子味比以及地球上预期的热中微子数量.
Rapid Variability and Broadband Spectral Modeling in the Flaring Activity of BL Lacertae
Yunnan University（云南大学）；Chinese Academy of Sciences（中国科学院）；Zhejiang Normal University（浙江师范大学）；Yunnan Normal University（云南师范大学）；Leshan Normal University（乐山师范学院）
