3C 105和3C 445热点区的复杂粒子加速过程
Complex particle acceleration processes in the hotspots of 3C105 and 3C445
摘要：
我们研究了低功率射电热点3C 105 South和3C 445 South的宽带辐射的性质。两个热点区域都在多个无线电/光学组件中解析。高灵敏度的无线电VLA，近红外/光学VLT和HST，和X射线钱德拉数据已被用来构建多波段光谱的个别热点组件。这两个热点区域的射电-光学光谱与一个同步加速器模型很好地拟合，该模型具有陡峭的光谱指数~0.8，断裂频率为10^12-10^14 Hz。3C 105南被分解为两个光学分量：一个主要的，对准喷流方向，可能标志着第一次喷流与周围介质的影响，和一个次要的，进一步从喷流，并在垂直于它的方向延伸。这个次要区域被解释为一个飞溅点形成的相对论等离子体从主要热点偏转。3C 445南的射电和光学图像显示了一个壮观的10千秒差距的弧形结构，其特征是两个主要组成部分，并垂直于喷流方向。I和B波段的HST图像进一步将最亮的成分分解为细长的特征。在3C 105南和3C 445南的主要热点组件被几个kpcs尺度的漫射光发射所掩盖，这表明可能在强地震中注入的非常高能量的粒子通过额外的加速机制在原地不断地再加速。我们认为，随机过程，与湍流和不稳定性，可以提供所需的额外的再加速。
英文摘要：
We investigate the nature of the broad-band emission associated with the low-power radio hotspots 3C105 South and 3C445 South. Both hotspot regions are resolved in multiple radio/optical components. High-sensitivity radio VLA, NIR/optical VLT and HST, and X-ray Chandra data have been used to construct the multi-band spectra of individual hotspot components. The radio-to-optical spectra of both hotspot regions are well fitted by a synchrotron model with steep spectral indices ~0.8 and break frequencies 10^12-10^14 Hz. 3C105 South is resolved in two optical components: a primary one, aligned with the jet direction and possibly marking the first jet impact with the surrounding medium, and a secondary, further out from the jet and extended in a direction perpendicular to it. This secondary region is interpreted as a splatter-spot formed by the deflection of relativistic plasma from the primary hotspot. Radio and optical images of 3C445 South show a spectacular 10-kpc arc-shape structure characterized by two main components, and perpendicular to the jet direction. HST images in I and B bands further resolve the brightest components into thin elongated features. In both 3C105 South and 3C445 South the main hotspot components are enshrouded by diffuse optical emission on scale of several kpcs, indicating that very high energy particles, possibly injected at strong shocks, are continuously re-accelerated in situ by additional acceleration mechanisms. We suggest that stochastic processes, linked to turbulence and instabilities, could provide the required additional re-acceleration.
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