【摘要】：冕羽是日冕中出現(xiàn)的明亮細(xì)長(zhǎng)的噴射結(jié)構(gòu),其足點(diǎn)扎根于色球?qū)?向上延伸到高日冕-行星際太陽風(fēng)區(qū)域。有觀測(cè)表明,冕羽可能與太陽風(fēng)的形成有密切的聯(lián)系,因此對(duì)冕羽形成與演化過程的深入研究有助于我們理解初始太陽風(fēng)的形成機(jī)制。冕羽足點(diǎn)在光球、色球以及日冕上對(duì)應(yīng)的活動(dòng)現(xiàn)象是了解冕羽形成和演化背后物理機(jī)制的重要載體。已有的研究證實(shí),冕羽的足點(diǎn)都對(duì)應(yīng)著光球上單極性主導(dǎo)的混合極性磁結(jié)構(gòu),且其中存在磁對(duì)消現(xiàn)象。在色球上,冕羽被發(fā)現(xiàn)與色球網(wǎng)絡(luò)結(jié)構(gòu)有關(guān),最近的一些研究還發(fā)現(xiàn)冕羽根部存在很多小噴流和冕羽瞬時(shí)增亮事件。另一方面,冕羽與日冕亮點(diǎn)間的聯(lián)系也是人們關(guān)心的另外一個(gè)問題,相關(guān)研究發(fā)現(xiàn)并不是所有的冕羽都有日冕亮點(diǎn)對(duì)應(yīng)。已有的研究工作主要關(guān)心冕羽與光球、色球和日冕內(nèi)特定的活動(dòng)現(xiàn)象之間對(duì)應(yīng)關(guān)系的存在性,對(duì)兩者間動(dòng)態(tài)演化過程的對(duì)應(yīng)性還沒有較明確的結(jié)論。我們的工作瞄準(zhǔn)相關(guān)研究中尚未完備的地方,著重研究冕羽的動(dòng)態(tài)演化過程及其與其它太陽大氣層次上發(fā)生的動(dòng)態(tài)等離子體現(xiàn)象之間的關(guān)聯(lián)。利用SDO觀測(cè)的連續(xù)性優(yōu)點(diǎn),結(jié)合其色球和日冕波段的成像以及光球縱向磁場(chǎng)數(shù)據(jù),我們分析了 15個(gè)冕羽的形成和動(dòng)態(tài)演化過程與動(dòng)態(tài)的光球磁活動(dòng)、色球活動(dòng)以及日冕亮點(diǎn)之間的關(guān)聯(lián)。首先,通過對(duì)AIA圖像分析,我們發(fā)現(xiàn)在冕洞內(nèi)幾乎所有單極磁場(chǎng)聚集區(qū)域都會(huì)存在冕羽,只是這些冕羽出現(xiàn)的亮度有所不同,這和以往EIT觀測(cè)有所不同,其原因主要是AIA儀器具有更高的觀測(cè)靈敏度。進(jìn)一步通過跟蹤冕羽及其對(duì)應(yīng)的光球磁場(chǎng)的動(dòng)態(tài)演化過程,發(fā)現(xiàn)冕羽形成過程對(duì)應(yīng)著根部主極性磁場(chǎng)與周圍同極性磁場(chǎng)匯聚的過程。我們還發(fā)現(xiàn)冕羽輻射強(qiáng)度最大時(shí)刻與匯聚的磁通量最大時(shí)刻有時(shí)間延遲,而冕羽輻射最強(qiáng)時(shí)刻往往與磁對(duì)消過程相對(duì)應(yīng)。其次,利用SDO/AIA 304 A的觀測(cè),我們發(fā)現(xiàn)冕羽根部與扎根于色球網(wǎng)絡(luò)場(chǎng)中的針狀體位置一致,且巨型針狀體可以引起冕羽的顯著增亮。這些巨型針狀體結(jié)構(gòu)同時(shí)對(duì)應(yīng)著主極場(chǎng)與周圍浮現(xiàn)的相反極性磁結(jié)構(gòu)的對(duì)消過程。這些磁對(duì)消活動(dòng)對(duì)應(yīng)的巨型針狀體雖然只持續(xù)幾分鐘到十幾分鐘,但卻可以維持冕羽數(shù)小時(shí)的增亮,與預(yù)計(jì)的輻射冷卻時(shí)標(biāo)相符�；谏鲜鲇^測(cè)事實(shí),我們認(rèn)為冕羽的形成與開放磁結(jié)構(gòu)的匯聚過程有關(guān),而小尺度的磁對(duì)消活動(dòng)(很可能對(duì)應(yīng)著磁重聯(lián))關(guān)聯(lián)的巨型針狀體活動(dòng)是導(dǎo)致并維持冕羽持續(xù)增亮的原因之一。最后,我們研究了日冕亮點(diǎn)與冕羽之間的關(guān)系,發(fā)現(xiàn)日冕亮點(diǎn)與冕羽的形成與演化有密切的關(guān)系,但不是一一對(duì)應(yīng)關(guān)系。在冕羽根部存在日冕亮點(diǎn)的情況下,日冕亮點(diǎn)存在時(shí)間內(nèi)伴隨的小尺度爆發(fā)現(xiàn)象可以引起冕羽的顯著增亮。然而并不是所有的冕羽根部都存在日冕亮點(diǎn)。綜上,我們的數(shù)據(jù)分析結(jié)論表明,開放磁結(jié)構(gòu)的匯聚是形成冕羽主體的基本物理過程,而影響冕羽演化的等離子體活動(dòng)都與冕羽主極場(chǎng)和相反極性磁結(jié)構(gòu)的對(duì)消過程有關(guān)。這些等離子體活動(dòng)可能是發(fā)生在色球?qū)拥木扌歪槧铙w噴流,也可能是發(fā)生在日冕中與日冕亮點(diǎn)有關(guān)的等離子體噴流。
[Abstract]:The coronal plume is a bright and elongated spray structure appearing in the corona. Its foot points are rooted in the chromosphere and extending upward to the high coronal interplanetary solar wind region. Observations show that the coronal plume may be closely related to the formation of the solar wind, so the deep study of the formation and evolution of the coronal plume will help us to understand the formation of the initial solar wind. Mechanism. The activity of the coronal plume at the photosphere, the chromosphere and the corona is an important carrier for understanding the physical mechanism behind the formation and evolution of the coronal plumes. The existing studies have confirmed that the feet of the coronal plumes are all corresponding to the unipolar mixed polar magnetic structure on the photosphere, and there is a magnetic cancellation phenomenon. The structure of the ball network is related. Some recent studies have found that there are many small jet and instantaneous brightening events in the coronal roots. On the other hand, the relationship between the coronal feather and the coronal highlights is another concern. The related research finds that not all coronal feathers have coronal highlights. The main concern of the existing research work is of concern. The correspondence between the coronal feathers and the photosphere, the chromosphere and the specific activity in the corona has no definite conclusion on the correspondence of the dynamic evolution processes between the two. Our work aims to focus on the dynamic evolution process of the coronal plumes and the occurrence of the evolution of the coronal feathers and the other solar atmosphere levels. Dynamic plasma shows the correlation between images. Using the continuity advantage of SDO observation, combining with the imaging of the chromosphere and coronal band and the longitudinal magnetic field data of the photosphere, we analyze the formation and dynamic evolution of the 15 coronal feathers, the dynamic photomagnetic activity, the correlation between the chromosphere activity and the coronal highlights. First, the AIA diagram is passed. Like analysis, we found that almost all the monopole magnetic field aggregation regions in the coronal cavity have coronal plumes, but the luminance of these coronal feathers is different, which is different from the previous EIT observations. The main reason is that the AIA instrument has higher observational sensitivity. The dynamic evolution of the coronal plume and its corresponding optical sphere magnetic field is further developed. It is found that the formation process of the coronal plume corresponds to the process of convergence between the main polar magnetic field of the root and the surrounding magnetic field. We also found that the maximum time for the maximum radiation intensity of the coronal plume and the maximum flux of the converged flux has time delay, and the strongest time of the coronal plume is often corresponding to the magnetic cancellation process. Secondly, we use the observation of SDO/AIA 304 A. The coronal root is in accordance with the position of the acicular body that is rooted in the chromosphere network field, and the giant needles can cause a significant brightening of the coronal plumes. These Mega acicular structures simultaneously correspond to the opposite polarity magnetic structure of the main pole field and the surrounding floating polarity. On the basis of the above observations, we believe that the formation of coronal feathers is related to the converging process of the open magnetic structure, and the mega acicular activity associated with the small scale magnetic cancellation activity (probably corresponding to the magnetic Reunion) leads to and maintains the crown based on the above observations. In the end, we have studied the relationship between the coronal highlights and the coronal plumes, and found that the coronal highlights are closely related to the formation and evolution of the coronal feathers, but not a one-to-one correspondence. In the case of coronal highlights in the coronal roots, the small scale eruptions associated with the time of the coronal highlights can be caused. However, the coronal highlights are not present in all the coronal plumes. To sum up, our data analysis shows that the convergence of the open magnetic structure is the basic physical process to form the main body of the coronal plume, and the plasma activity affecting the evolution of the coronal feathers is related to the elimination process of the main pole field of the coronal plume and the opposite polarity magnetic structure. These plasma activities may be large needle like exhales occurring in the chromosphere, or the plasma jet related to the coronal highlights in the corona.
【學(xué)位授予單位】：山東大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2017
【分類號(hào)】：P182

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 Fang-Ran Jiao;Li-Dong Xia;Zheng-Hua Huang;Bo Li;Hui Fu;Ding Yuan;Kalugodu Chandrashekhar;;Damping and power spectra of quasi-periodic intensity disturbances above a solar polar coronal hole[J];Research in Astronomy and Astrophysics;2016年06期

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本文編號(hào)：2151869