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Transition Region Blinkers – I. Quiet-Sun Properties

机译：过渡区域闪烁体– I.安静的太阳属性

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摘要

An automated method of identifying transition region blinkers is presented. The distribution and general properties of blinkers identified in the quiet Sun are discussed. The blinkers are seen most clearly in the O v (629 Å) transition region emission line, but they also have strong signatures in O iv (554 Å), and the chromospheric line, He i (584 Å). The strongest O v blinkers can also be identified in O iii (599 Å). No significant signatures are found for blinkers in the Mg ix (368 Å) and Mg x (624 Å) coronal lines. A few hundred O v blinkers are analyzed. Their global frequency is between 1 and 20 s−1 depending on how significant the peaks of the blinkers are. They have a typical area of 3×107 km2, a typical lifetime of 16 min and a typical intensity enhancement factor of 1.8. We find the ratios of the oxygen lines to be flat confirming the result that blinkers are not temperature events, but are density enhancements or due to increases in filling factor. Blinkers are found to occur preferentially over regions of enhanced chromospheric or transition region emission such as network boundaries, however, it is not so clear that they appear below the brightest coronal regions. A rough analysis of the magnetic fragments show that blinkers preferentially occur above regions where there are large or strong magnetic fragments with 75% occurring in regions where one polarity dominates.
机译：提出了一种识别过渡区域眨眼的自动方法。讨论了在安静的太阳下识别出的眨眼信号的分布和一般特性。在O v（629Å）过渡区域发射线中可以最清楚地看到眨眼，但它们在O iv（554Å）和色球线He i（584Å）中也具有很强的特征。还可以在O iii（599Å）中识别出最强的O v信号灯。在Mg ix（368Å）和Mg x（624Å）冠状线上没有发现明显的信号灯。分析了几百个O v信号灯。它们的整体频率在1到20 s-1 之间，具体取决于闪烁灯的峰值的重要性。它们的典型面积为3×107 km2 ，典型寿命为16分钟，典型强度增强因子为1.8。我们发现氧气线的比例是平坦的，这证实了眨眼不是温度事件，而是密度增加或由于填充因子增加而导致的结果。发现闪烁体优先出现在色球层或过渡区域发射增强的区域（例如网络边界）上方，但是，尚不清楚它们出现在最亮的日冕区域下方。对磁性碎片的粗略分析显示，眨眼优先出现在较大或较强磁性碎片的区域上方，其中75％的磁性在一个极性占主导的区域中发生。

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  • 来源
    《Solar Physics》 |2002年第1期|21-43|共23页
  • 作者

    D. Bewsher; C.E. Parnell; R.A. Harrison;

  • 作者单位

    Mathematical Institute University of St Andrews;

    Mathematical Institute University of St Andrews;

    Space Science Department Rutherford Appleton Laboratory;

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