冕洞是太阳日冕中的低温度、低密度和低辐射的区域，是高速太阳风的源 区。它们在上世纪中期就已经被人们所注意。虽然已经被研究了很多年，但是 对冕洞的认识还不是很深入，仍然存在着很多未解决的问题。随着各种高时间 和高空间分辨率的望远镜投入运行，系统且详细地分析冕洞成为可能。本论文 结合太阳动力学天文台（SDO；Solar Dynamic Observatory）以及全球日震观 测网（GONG；Global Oscillation Network Group）提供的资料，主要分析了 冕洞与活动区以及激活暗条之间的相互作用，以期待更深入地了解冕洞的特征 及本质。论文的主要研究结果归纳如下： 1. 利用SDO上搭载的大气成像组件（AIA；Atmospheric Imaging Assembly）以及 日震和磁像仪（HMI；Helioseismic and Magnetic Imager）的观测资 料，我们研究了2010年6月7日发生在一个孤立冕洞和一个新浮活动区之间的磁 相互作用。主要的观测结果如下：（1）随着新浮活动区的膨胀，亮环逐渐形成 在了冕洞和活动区之间，这些环连接着冕洞的负极性磁场与活动区的正极性 磁场。（2）随着亮环的形成，冕洞发生了及时的改变。它的东部边缘不断地 后退并且面积持续地衰减。（3）在冕洞边缘后退的过程中，两个日冕变暗区 域分别出现在了活动区的负极性磁场附近以及亮环的东部边缘，并且活动区 在一定程度上被扰动了。（4）随着亮环的形成，多个极紫外（EUV；extreme ultraviolet）喷流和一个弧形增亮出现在了冕洞的东部边缘。通过把这些观测 结果与外推的日冕磁场结构作对照，我们认为冕洞和活动区之间的相互作用很 好地符合了交换磁重联的模型，而这些观测结果则代表了交换磁重联的观测证 据。 2. 2010年11月13日，一个宁静暗条激活被观测到了。这个激活的暗条向 着一个中纬度冕洞的方向运动，遇到并且与这个冕洞发生了相互作用。借助 于AIA 、 HMI和GONG H 提供的数据，我们呈现了这个相互作用的详细的过 程。这个宁静暗条位于冕洞的西北方。它经历了一个非径向的激活，在激活的 过程中，暗条物质不断地从它的东部端点下落并且逐步入侵了冕洞。结果，冕 洞很明显地被这个入侵破坏了。增亮出现在了冕洞的西部边缘和内部，同时， 冕洞的西部边缘开始后退并且面积逐渐地衰减。当暗条物质停止下落的时候， 原来冕洞的大部分已经消失了。然而，剩余的冕洞部分却继续衰减并且最终 完全消失了。在暗条激活的过程中，三个日冕变暗区域（D1-D3）形成了，其 中D1和D2持续存在了冕洞消失的整个过程。外推的日冕磁场结构显示，宁静 暗条正位于一个较大的磁拱下面并且这个磁拱明显地连接着D1和D2 。通过对 照这个外推的结果，我们的观测表明，冕洞与激活暗条之间的相互作用涉及到 了暗条物质对冕洞的直接的入侵，并且冕洞的消失有可能来源于膨胀的磁拱和 冕洞的开场之间的交换磁重联。; Coronal holes（CHs）are regions with low temperature, low density and low emission in the solar corona, and they are the sources of fast solar wind. CHs have been noticed since the middle of the 20th century. Though studied for many years, the knowledge for them is still shallow, and there are many unresolved problems. As the telescopes with higher temporal and spatial resolution run, it becomes possible to study CHs in detail. In this paper, combining with the observations from the Solar Dynamic Observatory (SDO) and Global Oscillation Network Group (GONG), we analyze interactions of CHs with active region (AR) and activating filament, trying to understand the property and nature for CHs. The main results in this paper are summarized as follows: 1)By using the data from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI) on board the SDO, we study a magnetic interaction between an isolated CH and an emerging AR occurring on 2010 June 7. The main observational results are as follows: (1) Following the expansion of the AR, bright loops which linked the negative magnetic field of the CH to the positive polarity of the AR formed between the AR and the CH. (2) The CH changed seasonably as the bright loops formed. Its east boundaries constantly retreated and the area persisted in shrinking. (3) During the retreat of the CH boundaries (CHBs), two coronal dimmings respectively appeared at the negative polarity of the AR and the east boundaries of the bright loops，and the AR was partly disturbed. (4) The formation of the bright loops was accompanied by many extreme ultraviolet (EUV) jets and an arc-shaped brightening appearing at the CHBs. By comparing the observations with the derived coronal magnetic configuration, we think that the interaction between the CH and the AR excellently agreed with the model of interchange reconnection and these observational results represent evidence of interchange reconnection. 2. On 2010 November 13, an activation of a quiescent filament was observed. The activating filament moved towards a mid-latitude CH, met and interacted with it. Using the data from AIA, HMI and GONG H , we present the detail process of the interaction. The quiescent filament was located at the northwest of the CH. It underwent a nonradial activation, during which filament material constantly fell from its east end and gradually invaded into the CH. As a result, the CH was clearly destroyed by the intrusion. Brightenings appeared at the west boundaries and in the interior of the CH, meanwhile, its west boundaries began to retreat and the area gradually shrank. The major part of the CH disappeared when filament material stopped to fall. However, the rest of the CH went on shrinking and finally disappeared completely. During the filament activation, three coronal dimmings (D1-D3) were formed, among which D1 and D2 persisted throughout the whole disappearance of the CH. The derived coronal magnetic configuration shows that, the quiescent filament was located below a large magnetic arcade which obviously linked D1 to D2. By comparison with this result of extrapolation, our observations imply that the interaction between the filament and the CH involved direct intrusion of the filament material to the CH and the disappearance of the CH might be duo to the interchange reconnection between the expanding loop system and the CH’s open field.
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