论文标题
在宁静的地区爆发的灯丝下的光球流的演变
Evolution of photospheric flows under an erupting filament in the quiet-Sun region
论文作者
论文摘要
我们研究了大型安静的灯丝区域中太阳大气的动力学，该区域于2010年10月21日爆发。细丝爆发始于其北端，并在几个小时内从H $α$ line-line-Line-core核心滤清器线上消失。 AIA以紫外线记录了北腿的非常快的动作。 我们的目标是研究各种可用的数据集，描述了细丝爆发近五天的太阳大气的动力学。该间隔涵盖了细丝演变的三天，即细丝生长的前一天和喷发前一天。我们寻找导致细丝爆发的可能触发因素。 通过时间距离的气旋学和相干结构跟踪测量细丝区域中的表面速度场。通过跟踪30.4 nm AIA观测值的特征来估算较高大气中的明显速度。为了捕获磁场的演变，我们推断了光线视线线图，还计算了磁场的衰减指数。 我们发现光球速度场表现出一些特殊性。在细丝激活之前，我们观察到融合流向细丝脊柱的时间增加。另外，平均平方速度在激活前暂时增加，并在其之前达到峰值，然后急剧下降。我们进一步看到细丝区域中纬向流量成分的平均剪切幅度增加，然后急剧下降。 Photopheric L.O.S.磁场显示从细丝脊柱向东的感应持续增加。高度约10毫米的磁场的衰减指数显示出比北丝端连接点大于关键的值。
We studied the dynamics of the solar atmosphere in the region of a large quiet-Sun filament, which erupted on 21 October 2010. The filament eruption started at its northern end and disappeared from the H$α$ line-core filtergrams line within a few hours. The very fast motions of the northern leg were recorded in ultraviolet light by AIA. We aim to study a wide range of available datasets describing the dynamics of the solar atmosphere for five days around the filament eruption. This interval covers three days of the filament evolution, one day before the filament growth and one day after the eruption. We search for possible triggers that lead to the eruption of the filament. The surface velocity field in the region of the filament were measured by means of time-distance helioseismology and coherent structure tracking. The apparent velocities in the higher atmosphere were estimated by tracking the features in the 30.4 nm AIA observations. To capture the evolution of the magnetic field, we extrapolated the photospheric line-of-sight magnetograms and also computed the decay index of the magnetic field. We found that photospheric velocity fields showed some peculiarities. Before the filament activation, we observed a temporal increase of the converging flows towards the filament's spine. In addition, the mean squared velocity increased temporarily before the activation and peaked just before it, followed by a steep decrease. We further see an increase in the average shear of the zonal flow component in the filament's region, followed by a steep decrease. The photospheric l.o.s. magnetic field shows a persistent increase of induction eastward from the filament spine. The decay index of the magnetic field at heights around 10 Mm shows a value larger than critical at the connecting point of the northern filament end.
