Does Nearby Open Flux Affect the Eruptivity of Solar Active Regions?
Does Nearby Open Flux Affect the Eruptivity of Solar Active Regions?
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DOI：
10.3847/1538-4357/aac77a
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发表时间：
2018-02
期刊：
影响因子：
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通讯作者：
M. DeRosa;G. Barnes
中科院分区：
文献类型：
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作者：
M. DeRosa;G. Barnes
能量最高的太阳耀斑通常与日冕物质云以日冕物质抛射(CME)的形式射入日球层有关。然而，大型耀斑的存在并不伴随着CME。这些非爆发耀斑的存在提出了这样一个问题，即这些耀斑是否因为无法进入耀斑(重新连接)地点上方附近的开阔地带而受到影响。在这项研究中，我们使用太阳黑子第23周和第24周的56个耀斑样本来测试根据势场源-表面模型推断的产生爆发X级耀斑的活动区是否优先位于对日光层开放的日冕磁场区域附近。研究表明，可以进入开阔场地的X级耀斑爆发的速度比没有进入的速度更高。根据相关的贝叶斯因子，由于样本中有少量非爆发的X级耀斑，这一结果的重要性应该得到缓和。
The most energetic solar flares are typically associated with the ejection of a cloud of coronal material into the heliosphere in the form of a coronal mass ejection (CME). However, large flares exist that are not accompanied by a CME. The existence of these noneruptive flares raises the question of whether such flares suffer from a lack of access to nearby open fields in the vicinity above the flare (reconnection) site. In this study, we use a sample of 56 flares from sunspot Cycles 23 and 24 to test whether active regions that produce eruptive X-class flares are preferentially located near coronal magnetic field domains that are open to the heliosphere, as inferred from a potential field source-surface model. The study shows that X-class flares with access to open fields are eruptive at a higher rate than those for which access is lacking. The significance of this result should be moderated due to the small number of noneruptive X-class flares in the sample, based on the associated Bayes factor.