论文标题
大规模出现的导致非典型黑子灯桥的形成
The formation of an atypical sunspot light bridge as a result of large-scale flux emergence
论文作者
论文摘要
我们使用来自太阳能天文台的全盘数据和来自邓恩太阳能望远镜（DST）的高分辨率数据的组合，以研究常规的太阳共和国中非典型光桥（LB）的形成，结构和演变。 LB是由于磁通量的出现而产生的，一个脚步扎根于父子黑子外面的孔中，该孔在LB之前出现约17小时。该孔的极性与黑子的极性相反，并以约0.4 km/s的速度退出。这伴随着外部半阴茎中伸长的磁通道的发展，该通道触发了LB到达内半月边界时的形成。 LB是一种几乎水平的结构，其田间强度约为1.2 kg，沿其整个长度表现出长寿命的光平移约0.85 km/s。LB的出现在大约13分钟后导致彩色和过渡区域的动态激增。我们从光谱线参数和He I处的DST数据中得出了LB的光球和色球结构，在1083 nm，Si I，Si i，1082.7 nm，Ca II，在854 nm处，在656 nm处的HALPHA，以及700 nm和430 nm和430 nm的Speckle Reconstructed Imainsing成像。 LB在光球中显示出细长的丝状形状，而没有侧向挤压。 Ca II IR的热反转显示LB比UMBRA高约600-800 k。 LB的不同部分升至400至700公里之间的高度。我们的结果表明，LB形成是通量出现事件的一部分，LB信封达到约29毫米的高度，然后在大约13小时后溶解。我们建议，在LBS中存在持久的，大规模的光球蓝移，这是区分通量出现事件和推翻无现场象征侵入的对流的最有可能的标准。
We use a combination of full-disk data from the Solar Dynamics Observatory and high-resolution data from the Dunn Solar Telescope (DST) to study the formation, structure, and evolution of an atypical light bridge (LB) in a regular sunspot. The LB results from the emergence of magnetic flux with one footpoint rooted in a pore outside the parent sunspot that appears about 17 hrs before the LB. The pore has a polarity opposite to that of the sunspot and recedes away from it at a speed of about 0.4 km/s. This is accompanied by the development of an elongated magnetic channel in the outer penumbra which triggers the formation of the LB when it reaches the inner penumbral boundary. The LB is a nearly horizontal structure with a field strength of about 1.2 kG that exhibits long-lived photospheric blue-shifts of about 0.85 km/s along its entire length.The emergence of the LB leads to dynamic surges in the chromosphere and transition region about 13 min later. We derived the photospheric and chromospheric structure of the LB in the DST data from spectral line parameters and inversions of He i at 1083 nm, Si i at 1082.7 nm, Ca ii IR at 854 nm and Halpha at 656 nm, and speckle-reconstructed imaging at 700 nm and 430 nm. The LB shows an elongated filamentary shape in the photosphere without lateral extrusions. The thermal inversion of Ca ii IR reveals the LB to be about 600-800 K hotter than the umbra. Different sections of the LB are elevated to heights between 400 and 700 km. Our results indicate that the LB formation is part of a flux emergence event with the LB envelope reaching a height of about 29 Mm before dissolving after about 13 hr. We suggest that the existence of persistent, large-scale photospheric blue-shifts in LBs is the most likely criterion to distinguish between flux emergence events and overturning convection in field-free umbral intrusions.
