论文标题
在黑子中超级倾向的演变
Evolution Of Super-Sonic Downflows In A Sunspot
论文作者
论文摘要
在众多黑子上方的过渡区光谱中观察到了超级传播下花。但是，迄今为止，几乎没有研究这些签名在日子内在时间尺度上的持久性比几个小时更长的时间。在这里，我们分析了AR 12526的铅黑子，以推断其内部发生的超声下流的特性和演变。分析了16次大型，密集的光栅扫描由虹膜采样。在2016年3月27日至2016年4月2日之间，这些rasters以离散时间跟踪了AR 12526的铅太阳点。还研究了2016年4月1日获得的静坐观察，以分析较短的时间尺度上超级倾向的演变。在空间结构和速度方面，超级传奇下流在这个黑子中都是可变的。 16次栅格扫描中有13台在SI IV1394Å线中显示了一些超感性下流的证据，共同空间与1400Å裂缝成像通道中检测到的持续的明亮结构，峰值速度为112 km S^{ - 1}在2016年3月29日记录的证据。空间结构与从SI IV1394Å线推断出的空间结构不同。在坐姿数据数据中，最初未检测到双重流，但是，在60分钟后确实会发展出超声的下流。在观察结束前20分钟的时间里，这种下降从73 km s^{ - 1}加速到接近80 km s^{ - 1}。这些下流的形态在小时和几天的过程中演变出来，并且在SI IV1394Å和O IV1401Å线上通常是不同的。这些事件被发现在Si IV1394Å线核心的一个明亮区域的共同空间中，该区域似乎在冠状风扇循环的脚步处形成。
Super-sonic downflows have been observed in transition region spectra above numerous sunspots; however, little research has been conducted to date into how persistent these signatures are within sunspots on time-scales longer than a few hours. Here, we analyse the lead sunspot of AR 12526 to infer the properties and evolution of super-sonic downflows occurring within it. Sixteen large, dense raster scans sampled by IRIS are analysed. These rasters tracked the lead sunspot of AR 12526 at discrete times between the 27th March 2016 and the 2nd April 2016. One sit-and-stare observation acquired on the 1st April 2016 is also studied in order to analyse the evolution of super-sonic downflows on shorter time-scales. Super-sonic downflows are variable within this sunspot both in terms of spatial structuring and velocities. 13 of the 16 raster scans display some evidence of super-sonic downflows in the Si IV 1394 Å line co-spatial to a sustained bright structure detected in the 1400 Å slit-jaw imaging channel, with a peak velocity of 112 km s^{-1} being recorded on the 29th March 2016. Evidence for super-sonic downflows in the O IV 1401 Å line was found in 14 of these rasters, with the spatial structuring differing from that inferred from the Si IV 1394 Å line. In the sit-and-stare data, no dual flow is initially detected, however, a super-sonic downflow does develop after 60 minutes. This downflow accelerates from 73 km s^{-1} to close to 80 km s^{-1} in both the Si IV 1394 Å and O IV 1401 Å lines over the course of 20 minutes before the end of the observation. The morphology of these downflows evolved over the course of both hours and days and was often different in the Si IV 1394 Å and O IV 1401 Å lines. These events were found co-spatial to a bright region in the core of the Si IV 1394 Å line which appeared to form at the foot-points of coronal fan loops.
