Preflare Phenomena in Eruptive Flares
Preflare Phenomena in Eruptive Flares
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爆发性耀斑中的爆发前现象
DOI：
10.1086/378673
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发表时间：
2003
期刊：
影响因子：
--
通讯作者：
R. Canfield
中科院分区：
文献类型：
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作者：
Angela C. Des Jardins;R. Canfield
我们报告了一个统计研究的结果之间的关系爆发的太阳耀斑和观测到的Hα耀斑前的现象，我们称之为移动蓝移事件（MBSEs）。Hα的数据是使用Mees太阳观测站的CCD成像光谱仪（MCCD）收集的。我们的数据集中的16个事件都是由MCCD和Yohkoh软X射线望远镜观测到的，通常在耀斑发生前至少3小时，在某些情况下在耀斑发生前几天重复观测。数据集包含喷发和非喷发耀斑，没有偏见。集中在耀斑前后3小时的时间内，我们发现，在11次爆发性耀斑之前的MBSE的平均速率是5次非爆发性耀斑之前的约5倍。此外，MBSE的平均速率在爆发性耀斑之后下降了约6倍。早期的研究推断，MBSE反映了磁场重联后磁场重新调整产生的运动。从喷发耀斑和preflare MBSEs在几个小时前，这样的事件之间的高度相关性，我们得出结论，在色球层或低日冕的重连在建立导致太阳耀斑爆发的条件中起着重要的作用。
We report the results of a statistical study of the relationship between eruptive solar flares and an observed Hα preflare phenomenon we call moving blueshift events (MBSEs). The Hα data were gathered using the Mees Solar Observatory CCD imaging spectrograph (MCCD). The 16 events in our data set were observed by both the MCCD and the Yohkoh Soft X-Ray Telescope, typically for at least 3 hr prior to the flare and in some cases repeatedly for several days prior to the flare. The data set contains both eruptive and noneruptive flares, without bias. Focusing on 3 hr periods before and after the flares, we found that the average rate of MBSEs prior to the flares was ~5 times greater prior to the 11 eruptive flares than prior to the five noneruptive ones. Also, the average rate of MBSEs dropped by a factor of ~6 after the eruptive flares. Earlier studies inferred that MBSEs reflect motions that originate in the readjustment of magnetic fields after magnetic reconnection. From the high correlation between eruptive flares and preflare MBSEs in the several hours prior to such events, we conclude that reconnection in the chromosphere or low corona plays an important role in establishing the conditions that lead to solar flare eruptions.