论文标题
两次冠状质量弹出早期相互作用后的电子加速和无线电发射
Electron acceleration and radio emission following the early interaction of two coronal mass ejections
论文作者
论文摘要
语境。冠状质量弹出（CME）是来自太阳的磁化等离子体的大喷发，通常伴随着加速电子产生的太阳能无线电爆发。目标。加速电子束的强大来源是CME驱动的冲击，但是，在CME喷发期间，还有其他能够加速电子的机制。到目前为止，研究依赖于传统的太阳能无线电爆发分为五组（I型V），主要基于它们在动态光谱中的形状和特征。在这里，我们旨在确定与CME相关的移动无线电爆发的起源，该爆发不适合当前太阳能无线电发射。方法。 By using radio imaging from the Nançay Radioheliograph, combined with observations from the Solar Dynamics Observatory, Solar and Heliospheric Observatory, and Solar Terrestrial Relations Observatory spacecraft, we investigate the moving radio bursts accompanying two subsequent CMEs on 22 May 2013. We use three-dimensional reconstructions of the two associated CME eruptions to show the possible origin of the observed radio emission.结果。我们确定了位于CME北部侧面的电晕高度异常高的高度，并与CME同步向外移动。无线电爆发对应于动态光谱中的细胞结构发射，持续时间约为1 s，它们可能显示向前或反向频率漂移。由于CME在较早的CME之后紧密扩展，因此冠状CME-CME相互作用可能导致观察到的无线电发射。
Context. Coronal mass ejections (CMEs) are large eruptions of magnetised plasma from the Sun that are often accompanied by solar radio bursts produced by accelerated electrons. Aims. A powerful source for accelerating electron beams are CME-driven shocks, however, there are other mechanisms capable of accelerating electrons during a CME eruption. So far, studies have relied on the traditional classification of solar radio bursts into five groups (Type I-V) based mainly on their shapes and characteristics in dynamic spectra. Here, we aim to determine the origin of moving radio bursts associated with a CME that do not fit into the present classification of the solar radio emission. Methods. By using radio imaging from the Nançay Radioheliograph, combined with observations from the Solar Dynamics Observatory, Solar and Heliospheric Observatory, and Solar Terrestrial Relations Observatory spacecraft, we investigate the moving radio bursts accompanying two subsequent CMEs on 22 May 2013. We use three-dimensional reconstructions of the two associated CME eruptions to show the possible origin of the observed radio emission. Results. We identified three moving radio bursts at unusually high altitudes in the corona that are located at the northern CME flank and move outwards synchronously with the CME. The radio bursts correspond to fine-structured emission in dynamic spectra with durations of ~1 s, and they may show forward or reverse frequency drifts. Since the CME expands closely following an earlier CME, a low coronal CME-CME interaction is likely responsible for the observed radio emission.
