AI 中文总结
本研究利用南锡日冕射电日像仪的成像，确定未伴随CME的II型射电暴的精细结构起源于耀斑周边多区域，源区随激波非均匀移动，验证了激波在日冕传播时形成多射电源区的观点。
AI 中文摘要
日冕物质抛射等太阳爆发可驱动无碰撞激波，这类激波是良好的粒子加速器；由激波加速的电子会通过在低频射电波段产生的电磁辐射被远程观测到，太阳处激波加速电子的射电特征即为II型太阳射电暴，可用于追踪激波在日冕及更远处的传播。然而，II型射电暴在动态频谱中具有复杂形态，由大量精细时间与频率结构组成。本研究利用南锡日冕射电日像仪（Nançay Radioheliograph）的射电成像，确定构成II型射电暴的精细结构的位置与传播；研究的II型射电暴仅与某耀斑和日冕波时间重合，未伴随日冕物质抛射（CME），但仍呈现复杂形态。结果发现，构成该II型射电暴的辐射带与精细结构起源于耀斑位置周边的多个区域，源区还会随激波膨胀沿特殊的非均匀传播方向移动；该结果支持激波在日冕传播时会形成多个射电源区的观点。
英文摘要
Solar eruptions such as coronal mass ejections can drive collisionless shocks that are good particle accelerators. Electrons accelerated by these shocks can be observed remotely via the electromagnetic emission they generate at low radio frequencies. The radio signatures of shock-accelerated electrons at the Sun are type II radio bursts that can be used to track the propagation of the shock wave in the solar corona and beyond. However, type II radio bursts can have complex morphologies in dynamic spectra, being composed of numerous fine time and frequency structures. Here, we aim to determine the location and propagation of the fine structures composing type II bursts using radio imaging from the Nançay Radioheliograph. We investigate the origin of a type II radio burst that was only co-temporal with a flare and a coronal wave, and it was not associated with a CME eruption. The type II burst still showed complex morphology. We find that emission lanes and fine structures composing the type II burst originate from multiple locations around the flare site. The source regions also move in peculiar non-uniform propagation directions following the shock expansion. Our findings are consistent with the idea that multiple radio emission source regions form as a shock propagates through the solar corona.
Comments13 pages, 5 figures. Accepted for publication in the Planetary, Solar, and Heliospheric Radio Emissions X Proceedings
