ERUPTIONS FROM SOLAR EPHEMERAL REGIONS AS AN EXTENSION OF THE SIZE DISTRIBUTION OF CORONAL MASS EJECTIONS
ERUPTIONS FROM SOLAR EPHEMERAL REGIONS AS AN EXTENSION OF THE SIZE DISTRIBUTION OF CORONAL MASS EJECTIONS
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DOI：
10.1088/0004-637x/710/2/1480
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发表时间：
2009-12
期刊：
影响因子：
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通讯作者：
C. Schrijver
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文献类型：
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作者：
C. Schrijver
在171 Å （~ 1 MK）过渡带和日冕探测器（TRACE）对平静日冕的观测经常显示小规模短暂双极区日冕部分的中断，类似于更大规模的日冕物质抛射（cme）的现象：短暂区域表现出耀斑样的光亮，在色球温度下携带吸收物质的灯丝迅速上升，或周围日冕暂时变暗。我分析了1998年4月1日至2009年9月30日之间所有可用的TRACE观测序列，使用全分辨率171 Å图像序列，在距离磁盘中心500弧秒的范围内跨度一天或更长时间，以良好的曝光和相对较低的背景观测到安静的太阳。在2000年至2008年之间确定了10个这样的数据集，跨越了570小时的观测，总共暴露了17,133次。确定了80次小规模日冕爆发。它们的大小分布形成了日冕物质抛射角宽度分布的平滑延伸，表明双极磁区的喷发频率基本上在至少2个数量级上是无标度的，从接近TRACE弧秒分辨率极限的喷发到内日球层观测到的最大日冕物质抛射。这个尺度范围可能与磁场中嵌套的一系列连通性范围的性质有关，在这些连通性范围中，越来越大的高能事件可以越来越高地进入日冕，直到到达日球层。
Observations of the quiet solar corona in the 171 Å (∼1 MK) passband of the Transition Region and Coronal Explorer (TRACE) often show disruptions of the coronal part of small-scale ephemeral bipolar regions that resemble the phenomena associated with coronal mass ejections (CMEs) on much larger scales: ephemeral regions exhibit flare-like brightenings, rapidly rising filaments carrying absorbing material at chromospheric temperatures, or the temporary dimming of the surrounding corona. I analyze all available TRACE observing sequences between 1998 April 1 and 2009 September 30 with full-resolution 171 Å image sequences spanning a day or more within 500 arcsec of disk center, observing essentially the quiet Sun with good exposures and relatively low background. Ten such data sets are identified between 2000 and 2008, spanning 570 hr of observing with a total of 17,133 exposures. Eighty small-scale coronal eruptions are identified. Their size distribution forms a smooth extension of the distribution of angular widths of CMEs, suggesting that the eruption frequency for bipolar magnetic regions is essentially scale free over at least 2 orders of magnitude, from eruptions near the arcsecond resolution limit of TRACE to the largest CMEs observed in the inner heliosphere. This scale range may be associated with the properties of the nested set of ranges of connectivity in the magnetic field in which increasingly large and energetic events can reach higher and higher into the corona until the heliosphere is reached.