本文選題：太陽磁場 + 太陽活動��； 參考：《中國科學院研究生院（云南天文臺）》2014年博士論文

【摘要】：太陽磁場結構在太陽表面大氣層上表現為各種不同的空間尺度,目前國內外最先進的太陽觀測設備的衍射極限正在接近理論預言的最小磁場結構(磁元)的尺度范圍。觀測數據和數值模擬都揭示出太陽表面大氣層上的小尺度磁結構是無處不在的但并非是絕對的均勻分布,這些小尺度磁結構提供了太陽輻射絕大部分的能量來源。雖然它們不像劇烈耀斑爆發(fā)和日冕物質拋射具有極其壯觀的景象,但是不能忽視它們在太陽物理中的重要地位,因為它們對于認識和揭示太陽全球／局部湍流發(fā)電機理論、色球和日冕加熱機制、太陽風的起源和加速、磁流浮現與對消等還未完全理解的領域具有相當重要的科學意義。 近半個世紀以來,對太陽小尺度磁結構的研究是太陽物理領域中一項被普遍關注且高度重視的前沿課題之一。盡管太陽小尺度磁結構的觀測特征及其物理機制的研究已經在觀測和理論方面取得了很大的進展,但是絕大多數中等口徑的太陽觀測設備的高分辨率觀測數據是不對外公布的,這為太陽小尺度磁結構的深入研究制造了較大的障礙。從2011年開始,云南天文臺撫仙湖太陽觀測站的新真空太陽望遠鏡(New Vacuum Solar Telescope, NVST)對太陽進行常規(guī)觀測,其配備的高性能光球和色球終端設備以及即將投入使用的多通道觀測終端、偏振分析器和多波段光譜儀,為我們研究太陽小尺度磁結構提供了前所未有的機遇。 本論文是將光球亮點和極區(qū)光斑兩種具有千高斯量級的光球小尺度磁結構作為研究對象,使用NVST的高分辨率光球觀測數據和日本國立天文臺(National Astronomical Observatory of Japan, NAOJ)的極區(qū)光斑時序數據分別對它們的觀測特征和統(tǒng)計特性進行細致的分析和研究。本論文的第一部分對太陽小尺度磁結構的研究背景、現狀和意義進行了綜述,并結合目前所能獲取的高分辨率觀測資料和長期的時間序列數據,由此提出論文的研究對象、內容和目標并展開研究。 論文的第二部分是采用NVST在TiO(氧化鈦)觀測波段于2012年10月29日和2013年5月21日采集的具有高時間高空間分辨率的光球觀測資料,首先提出一種拉普拉斯變換和形態(tài)學膨脹相結合的識別算法來準確快速的提取出光球亮點,然后對兩組觀測數據進行詳細的對比分析,并得出光球亮點的尺度、亮度、速度和形狀等多種特征參數,最后對這些觀測特征的相關性進行分析討論。研究結果表明：1)提出的識別算法可以有效的提取出光球亮點并能對其演化特性進行深入分析,而且該算法可以應用到太陽大氣其它層次上具有類似特征的小尺度亮結構上；2)光球亮點的尺寸與亮度分布具有較好的相關性,這表明NVST在光球波段的觀測性能達到了預期目標,也意味著TiO譜線形成于光球層較低的位置,因此光球亮點的亮度與平均光球強度的反差要小于光球中高層的對比度；3)光球亮點的速度分布和形狀變化(偏心率)的相關性可能與磁流管內的物質流動有關,這對于揭示光球亮點的振蕩所激發(fā)的阿爾芬波將磁能從光球向色球和日冕傳輸并對高層大氣進行加熱有著積極的意義。 論文的第三部分是結合傳統(tǒng)的線性分析工具和先進的非線性分析技術來研究極區(qū)光斑和黑子活動的長期時序數據的統(tǒng)計特性,主要是探索太陽高緯和低緯區(qū)域活動指標的周期演化、相位異步、空間分布和混沌分形等特征的異同性。研究結果表明：1)極區(qū)光斑在高頻范圍內的準周期數量多于低頻范圍內的數量,而且兩個半球上的準周期值存在細微的差別,可能是由太陽活動的空間分布特性引起的；2)太陽高緯指數與低緯活動指標存在半個活動周的相位異步關系,但是在太陽活動周的不同相和不同半球上的表現并不一致；3)兩者的空間分布都存在半球不同時性和不對稱性,但是在不同的緯度區(qū)域表現出完全不同的特征；4)兩者具有類似的低維混沌效應,但是分形維數與長程相關性略有不同,意味著它們在太陽活動中短期預報的準確性方面是不同的。這些分析結果都表明兩者所表征的不同磁場本質是導致它們的統(tǒng)計特征既存在相似性又存在差異性的主要原因。 由于太陽小尺度磁結構在揭示太陽物理領域中多個還未完全理解的物理機制方面占有重要的科學地位,因此對其觀測特性和物理機制的探索將是一項在未來很長一段時間內仍需不斷研究的課題內容。針對光球亮點和極區(qū)光斑這兩種具有強磁場強度的小尺度亮結構,以后將對光球亮點的磁場復雜性和自相似性、活動周演化特性、振蕩行為和物質流動,并對高緯活動現象的極向漂移速率、光斑和亮點的交叉對比、光斑和譜斑的振蕩異同性等方面展開后續(xù)研究。相信這些研究工作對于約束太陽湍流發(fā)電機理論、認識高層大氣的加熱機制和探索快速太陽風的起源等領域具有重要的推動作用。
[Abstract]:The structure of the solar magnetic field shows a variety of spatial scales on the surface of the solar surface. The diffraction limit of the most advanced solar observation equipment at home and abroad is approaching the scale range of the smallest magnetic field structure (magnetic element) predicted by the theory. The observation data and numerical simulation reveal the small scale magnetic structure in the solar surface. The ubiquitous, but not absolute, uniform distribution, these small scale magnetic structures provide most of the energy sources of solar radiation. Although they are not as spectacular as violent flare eruptions and coronal mass ejections, they cannot ignore their importance in solar physics, because they are known and revealed. The theory of global / local turbulent generators of the sun, the mechanism of chromosphere and coronal heating, the origin and acceleration of the solar wind, the emergence of magnetic flow and the field that have not been fully understood are of considerable scientific significance.
For nearly half a century, the study of the small scale magnetic structure of the sun is one of the most concerned and highly valued topics in the field of solar physics. Although the observational characteristics and the physical mechanism of the solar small scale magnetic structure have made great progress in the field of observation and theory, but the vast majority of medium caliber The high resolution observation data of the solar observation equipment are not published, which makes a big obstacle to the deep study of the solar small scale magnetic structure. Since 2011, the new New Vacuum Solar Telescope (NVST) of the sun Observatory in Fuxian Lake, Yunnan Observatory, is equipped with a regular observation of the sun. High performance photosphere and chromosphere terminal equipment, and the upcoming multichannel observation terminal, polarization analyzer and multi band spectrometer provide unprecedented opportunities for us to study the small scale magnetic structure of the sun.
In this paper, the two kinds of small scale magnetic structures with the light ball and the polar spot are taken as the research objects. The observational features and statistics of the polar region temporal data of the high resolution optical sphere of NVST and the National Observatory (National Astronomical Observatory of Japan, NAOJ) of the Japanese National Observatory (Observatory of Japan, NAOJ) are observed respectively. The first part of this paper summarizes the research background, current situation and significance of the solar small scale magnetic structure, and combines the high resolution observation data and the long time series data that can be obtained at present, and then puts forward the research object, content and goal of the paper.
The second part of the paper is a high time and high spatial resolution optical sphere observation data collected by NVST in the TiO (titanium oxide) observation band in October 29, 2012 and May 21, 2013. First, a recognition algorithm combining Laplasse transform and morphological expansion is proposed to accurately and quickly extract light bulb bright spots, and then to two groups. The observation data are compared and analyzed in detail, and a variety of characteristic parameters such as the size, brightness, speed and shape of the bright ball bright spot are obtained. Finally, the correlation of these observation features is analyzed and discussed. The results show that: 1) the recognition algorithm can effectively extract the light bulb bright spot and can analyze its evolution characteristics deeply. And the algorithm can be applied to small scale bright structures with similar characteristics at other levels of the solar atmosphere; 2) the size of the bright light bulb has a good correlation with the distribution of luminance, which indicates that the observational performance of NVST in the light sphere reaches the desired target, which means that the TiO line is formed at a lower position in the photosphere, so the light sphere is bright. The contrast between the point brightness and the average ball strength is less than the contrast in the high layer in the light sphere; 3) the correlation between the velocity distribution and the shape change (eccentricity) of the bright ball bright spot may be related to the material flow in the magnetic flow tube, which is the transfer of the magnetic energy from the photosphere to the chromosphere and corona by the Alfan wave which reveals the oscillation of the bright ball bright spot. Heating in the upper atmosphere has a positive significance.
The third part of the thesis is to study the statistical characteristics of the long term ordinal numbers of polar spot and sunspot activities based on the traditional linear analysis tools and advanced nonlinear analysis techniques, mainly to explore the similarities and differences between the periodic evolution, Phase Asynchronism, space distribution and chaotic fractal of the activity indexes of the high and low latitude regions of the sun. The results show that: 1) the quasi periodic number of the polar spot in the high frequency range is more than the number of the low frequency range, and the quasi periodic values on the two hemispheres are slightly different, which may be caused by the spatial distribution of the solar activity; 2) the phase asynchronous relationship between the high latitude index and the low latitude active index exists in the phase of a half active week. However, the performance of different phases and different hemispheres in the solar cycle is not consistent; 3) there are hemispherical dissymmetry and asymmetry in the spatial distribution of the two, but there are completely different characteristics in different latitudes; 4) the two have similar low dimensional chaotic effects, but the fractal dimension is slightly different from the long range correlation. It means that they are different in the accuracy of the short term prediction in the solar activity. These results show that the nature of the different magnetic fields characterized by the two is the main cause of the similarity and difference in their statistical characteristics.
As the solar small scale magnetic structure occupies an important scientific position in revealing many unknown physical mechanisms in the field of solar physics, the exploration of its observation and physical mechanism will be a subject that still needs to be studied for a long time in the future. Two kinds of light ball bright spots and polar spot light spots are needed. The small scale bright structure with strong magnetic field strength will follow the following aspects, such as the complexity and self similarity of the magnetic field, the evolution characteristics of the active week, the oscillating behavior and the material flow, the extreme drift rate of the high latitude activity, the cross contrast of the spot and the bright spot, the oscillation of the spot and the spectrum of the speckle and so on. Some research work plays an important role in restricting the theory of the solar turbulence generator, understanding the heating mechanism of the high atmosphere and exploring the origin of the fast solar wind.
【學位授予單位】：中國科學院研究生院（云南天文臺）
【學位級別】：博士
【學位授予年份】：2014
【分類號】：P182

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相關期刊論文 前4條

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4 Zhong Liu;Jun Xu;Bo-Zhong Gu;Sen Wang;Jian-Qi You;Long-Xiang Shen;Ru-Wei Lu;Zhen-Yu Jin;Lin-Fei Chen;Ke Lou;Zhi Li;Guang-Qian Liu;Zhi Xu;Chang-Hui Rao;Qi-Qian Hu;Ru-Feng Li;Hao-Wen Fu;Feng Wang;Men-Xian Bao;Ming-Chan Wu;Bo-Rong Zhang;;New vacuum solar telescope and observations with high resolution[J];Research in Astronomy and Astrophysics;2014年06期

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本文編號：2044559