【作者】 张良；

【导师】 郑瑞生；

【作者基本信息】 山东大学 ， 地球物理， 2023， 硕士

【摘要】 太阳爆发会向太空抛射大量磁化等离子体和辐射高能粒子,从而影响空间天气,是空间天气变化的源头。剧烈的太阳爆发会影响到空间站人员的安全以及地球上的日常通信;因此,对于太阳爆发现象的观测研究有利于我们掌握太阳爆发的本质,从而更好地对空间天气变化做出预测。本文主要分为两个部分,首先对导致太阳爆发的暗条进行了研究,通过分析暗条从形成到形变/消退的特殊生命周期,提出当储存的磁能被逐渐释放时,暗条不会爆发,只会变形/消退这一观点。然后对伴随太阳爆发产生的极紫外波进行了研究,通过联系磁场与波产生的位置,对波的产生机制进行了更加深入的探索。在太阳暗条的观测研究中,利用SDO和SMART的高时间分辨率资料,研究了活动区(AR)12760中小暗条的形成和形变/消退过程。形成:暗条细丝以头尾磁重联的形式相互连接形成了活动区中拉长且剪切的目标暗条。在重联期间,底部磁场存在明显的磁活动(磁浮现,磁汇聚和磁对消),上层大气在重联时刻也产生突发的增亮,这可能暗示着暗条的形成与底部的磁活动密切相关;形变:暗条形成后与周围的一个小暗条发生多次磁相互作用,导致暗条的形变/消退。在日冕极紫外波的观测研究中,挑取了三个太阳喷流驱动的日冕极紫外波,旨在通过研究不伴随CME的弱喷流产生的波,探索喷流与爆发期间保持闭合的日冕环之间的具体相互作用过程,从而得出喷流波的驱动机制。结合光球层磁场信息和势场外推方法,量化了日冕环上的磁场强度分布,通过对比日冕环上磁场强度最弱的位置和波的产生位置,得出喷流倾向于作用在日冕环上磁场强度最弱的部分,以至于波在这部分前面产生的结论。更多还原

【Abstract】 Solar eruptions can release a large amount of plasma and magnetic field and thus lead to a significant disturbance for space weather,therefore affecting space weather.Violent solar eruptions can affect the safety of space station staff and daily satellite communication on Earth.Therefore,the observation of solar eruptions is beneficial for us to grasp the essence of solar eruptions and make better predictions of changes in space weather.This article is mainly divided into two parts.Firstly,it studies the filaments that cause solar eruptions.The opposite physical essence between filament deformation and filament eruptions was analyzed through a special life cycle of a small filament from formation to deformation.The second part is to study the extreme ultraviolet waves generated by solar eruptions.The driving mechanism of wave is explored more deeply by associating the magnetic field with the birth place of the wave.In the observation of solar filaments,the formation process of small filaments in AR12760 was studied using high-resolution observation from SDO and SMART.The elongated small filament is formed by multiple head tail magnetic reconnection between several filament threads.During reconnection,there existed significant magnetic evolution in the source region(magnetic emergence,magnetic convergence,and magnetic cancellation),and associated brightenings in the upper atmosphere.It likely suggests that the formation of small filament is closely related to the magnetic activity in the photosphere.In the observation of coronal extreme ultraviolet waves,three coronal extreme ultraviolet waves driven by solar jets were selected.The three waves were not associated with CMEs.It is to explore the specific interaction process between jet and overlying loops that remain close during the eruption and then provide insight for the driving mechanism of jet-driven waves.Combining magnetic field in the photosphere and PFSS method,the distribution of the magnetic field intensity of the overlying loops is quantified.Comparing the birth place of waves and the weakest part of the overlying loops,it is likely the jet prefer to interacted with the weakest part of the overlying loops.Therefore the wave was generated ahead of this part.更多还原