论文标题
在太阳喷发期间连续拉伸磁场结构触发的准周期性极端脉冲波的跨环繁殖
Cross-loop propagation of a quasi-periodic extreme-ultraviolet wave train triggered by successive stretching of magnetic field structures during a solar eruption
论文作者
论文摘要
太阳极端硫酸群（EUV）波通常是指EUV成像观测中太阳喷发部位向外传播的大规模干扰。使用船上太阳能动力学天文台（SDO）的大气成像组件（AIA）的最新观察结果，我们报告了一种准周期波列车，以$ \ sim $ 308 km $ 308 km s $ s $^{ - 1} $的平均速度向外传播。至少可以清楚地识别五个波前，这段时间为$ \ sim $ 120 s。这些波前源自冠状环的扩展，其速度明显的速度为$ \ sim $ 95 km s $^{ - 1} $，比波列慢了3倍。在没有强大横向膨胀的情况下，这些观察结果可以通过Chen等人的理论模型来解释。 （2002年），它预测EUV波可能具有两个组成部分：更快的组件是快速模式的磁声波或冲击波，并且由于连续拉伸封闭磁场线的伸展而形成的较慢的前沿。在这种情况下，我们观察到的波列和连续的循环扩展可能分别与模型中的快速和慢速组件相对应。
Solar extreme-ultraviolet (EUV) waves generally refer to large-scale disturbances propagating outward from sites of solar eruptions in EUV imaging observations. Using the recent observations from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO), we report a quasi-periodic wave train propagating outward at an average speed of $\sim$308 km s$^{-1}$. At least five wavefronts can be clearly identified with the period being $\sim$120 s. These wavefronts originate from the coronal loop expansion, which propagates with an apparent speed of $\sim$95 km s$^{-1}$, about 3 times slower than the wave train. In the absence of a strong lateral expansion, these observational results might be explained by the theoretical model of Chen et al. (2002), which predicted that EUV waves may have two components: a faster component that is a fast-mode magnetoacoustic wave or shock wave and a slower apparent front formed as a result of successive stretching of closed magnetic field lines. In this scenario, the wave train and the successive loop expansion we observed likely correspond to the fast and slow components in the model, respectively.
