太陽日珥震蕩的觀測和理論研究
發(fā)布時間：2018-10-09 08:21
【摘要】：太陽日珥震蕩常涉及多方面的太陽活動,包括活動區(qū)爆發(fā)(主要是耀斑和CME)及其所觸發(fā)的日冕波動傳播,以及引起鄰近日珥結(jié)構(gòu)震蕩的主要擾動EUV波。我們所研究的三列日珥震蕩事件是由同一日珥結(jié)構(gòu)在受到鄰近活動區(qū)爆發(fā)事件的作用下發(fā)生的,這一日珥結(jié)構(gòu)在序列擾動下的不同震蕩表現(xiàn)為研究有關(guān)物理機制提供了很好的機會。此外,對日珥震蕩參數(shù)的觀測分析已經(jīng)成為日珥冕震學(xué)測量磁場的一個重要手段。因此,對日珥震蕩的研究具有非常重要的科學(xué)意義。本文利用SDO/AIA的觀測數(shù)據(jù),分析了這三列日珥震蕩的產(chǎn)生以及運動特征,主要的內(nèi)容及結(jié)論如下：我們首先分析了震蕩驅(qū)動源—活動區(qū)處發(fā)生的相應(yīng)耀斑和CME事件,三次爆發(fā)都觀測到了M級的耀斑,其中后兩次爆發(fā)也伴隨有CME。在差分圖上可以觀測到后兩次CME驅(qū)動的EUV波前沿,根據(jù)CME爆發(fā)和日珥震蕩起始的時間差,我們計算了EUV波的傳播速度,并且確認EUV波是引起日珥震蕩的直接原因。對于第一次爆發(fā)在差分圖上沒有看到EUV波前沿,然而結(jié)合日冕波動傳播速度v=967±50 Km/s,我們猜測這列波動有可能對應(yīng)于耀斑驅(qū)動的莫爾頓波(Morten wave)或爆震波(blast wave).隨后我們對同一震蕩不同高度的日珥做切片,得到震蕩波形并且測量了它們的起始時間和周期振幅等參數(shù)。最后對三列日珥震蕩進行比較,確認它們的震蕩模式是集體kink震蕩。此外,我們還研究了horn的震蕩行為,同日珥震蕩做了比較,發(fā)現(xiàn)二者在周期振幅等參數(shù)上有很多不同,我們認為這是由于horn延伸入冕腔中,受到大尺度日冕磁場結(jié)構(gòu)的影響,因而表現(xiàn)出與日珥震蕩不同的觀測特征,據(jù)我們所知,這是首次報道的horn準周期震蕩現(xiàn)象。另外,我們對日珥震蕩的參數(shù)進行了擬合,主要是應(yīng)用一個衰減的正弦函數(shù)加上一個線性的漂移函數(shù),分別得到了三列震蕩的周期為25±2 min,36±2 min,28±2 min,振幅為2.62±1.0 arcsec,8.59±1.0 arcsec,9.07±1.0 arcsec和衰減時間120±20 min,145±20 min,165±10min,通過衰減時間,簡單的分析了日珥震蕩的衰減機制,同時計算了震蕩初始速度幅度,說明了這三列震蕩都是較大幅度的日珥震蕩。其次,我們利用日珥冕震學(xué)的一些模型估算了日冕磁場,所得結(jié)果與文獻中的已有數(shù)據(jù)相符。
[Abstract]:Solar prominence oscillations often involve many aspects of solar activity, including active zone bursts (mainly flares and CME) and the propagation of coronal waves triggered by them, as well as the main disturbed EUV waves that cause structural oscillations in adjacent prominence. The three rows of prominence oscillations we studied were caused by the same prominence structure under the influence of an outbreak in the adjacent active region. The different oscillations of this prominence structure under sequential disturbances provide a good opportunity to study the physical mechanism. In addition, the observation and analysis of the oscillation parameters have become an important means of measuring the magnetic field of the prominence coronal seismicity. Therefore, the study of prominence oscillation is of great scientific significance. Based on the observational data of SDO/AIA, the generation and motion characteristics of the three series of prominence oscillations are analyzed. The main contents and conclusions are as follows: firstly, we analyze the corresponding flares and CME events in the source-active region of the oscillation drive. M-level flares were observed in all three bursts, and the latter two were accompanied by CME.. The front of the last two CME driven EUV waves can be observed on the difference diagram. According to the time difference between the onset of the CME burst and the prominence oscillation, we calculate the propagation velocity of the EUV wave, and confirm that the EUV wave is the direct cause of the prominence oscillation. For the first burst, we do not see the front of the EUV wave on the difference diagram, but with the coronal wave propagation velocity vt 967 鹵50 Km/s, we speculate that this wave may correspond to the flare-driven Morton wave (Morten wave) or the detonation wave (blast wave). Then we slice the prominence of the same oscillation at different heights to obtain the oscillation waveforms and measure their starting time and periodic amplitude. Finally, three columns of prominence oscillations are compared and their oscillation patterns are confirmed to be collective kink oscillations. In addition, we also study the oscillatory behavior of horn and compare it with that of prominence oscillation. We find that there are many differences between them in terms of periodic amplitude and other parameters. We think this is due to the fact that horn extends into the coronal cavity and is affected by the structure of large-scale coronal magnetic field. Therefore, the observed characteristics are different from those of the prominence oscillation, which is the first reported phenomenon of horn quasi periodic oscillation as far as we know. In addition, we fit the parameters of the prominence oscillation, mainly by using a attenuated sinusoidal function and a linear drift function. The period of triplex oscillation is 25 鹵2 min,36 鹵2 min,28 鹵2 min, the amplitude is 2. 62 鹵1. 0 arcsec,8.59 鹵1. 0 arcsec,9.07 鹵1. 0 arcsec and the attenuation time is 120 鹵20 min,145 鹵20 min,165 鹵10. Through the attenuation time, the attenuation mechanism of prominence oscillation is simply analyzed, and the amplitude of initial velocity of oscillation is calculated. This shows that the three series of shocks are large amplitude of the prominence shock. Secondly, we estimate the coronal magnetic field by using some models of prominence coronal seismology, and the results are in agreement with the available data in the literature.
【學(xué)位授予單位】：山東大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P182
本文編號：2258641
[Abstract]:Solar prominence oscillations often involve many aspects of solar activity, including active zone bursts (mainly flares and CME) and the propagation of coronal waves triggered by them, as well as the main disturbed EUV waves that cause structural oscillations in adjacent prominence. The three rows of prominence oscillations we studied were caused by the same prominence structure under the influence of an outbreak in the adjacent active region. The different oscillations of this prominence structure under sequential disturbances provide a good opportunity to study the physical mechanism. In addition, the observation and analysis of the oscillation parameters have become an important means of measuring the magnetic field of the prominence coronal seismicity. Therefore, the study of prominence oscillation is of great scientific significance. Based on the observational data of SDO/AIA, the generation and motion characteristics of the three series of prominence oscillations are analyzed. The main contents and conclusions are as follows: firstly, we analyze the corresponding flares and CME events in the source-active region of the oscillation drive. M-level flares were observed in all three bursts, and the latter two were accompanied by CME.. The front of the last two CME driven EUV waves can be observed on the difference diagram. According to the time difference between the onset of the CME burst and the prominence oscillation, we calculate the propagation velocity of the EUV wave, and confirm that the EUV wave is the direct cause of the prominence oscillation. For the first burst, we do not see the front of the EUV wave on the difference diagram, but with the coronal wave propagation velocity vt 967 鹵50 Km/s, we speculate that this wave may correspond to the flare-driven Morton wave (Morten wave) or the detonation wave (blast wave). Then we slice the prominence of the same oscillation at different heights to obtain the oscillation waveforms and measure their starting time and periodic amplitude. Finally, three columns of prominence oscillations are compared and their oscillation patterns are confirmed to be collective kink oscillations. In addition, we also study the oscillatory behavior of horn and compare it with that of prominence oscillation. We find that there are many differences between them in terms of periodic amplitude and other parameters. We think this is due to the fact that horn extends into the coronal cavity and is affected by the structure of large-scale coronal magnetic field. Therefore, the observed characteristics are different from those of the prominence oscillation, which is the first reported phenomenon of horn quasi periodic oscillation as far as we know. In addition, we fit the parameters of the prominence oscillation, mainly by using a attenuated sinusoidal function and a linear drift function. The period of triplex oscillation is 25 鹵2 min,36 鹵2 min,28 鹵2 min, the amplitude is 2. 62 鹵1. 0 arcsec,8.59 鹵1. 0 arcsec,9.07 鹵1. 0 arcsec and the attenuation time is 120 鹵20 min,145 鹵20 min,165 鹵10. Through the attenuation time, the attenuation mechanism of prominence oscillation is simply analyzed, and the amplitude of initial velocity of oscillation is calculated. This shows that the three series of shocks are large amplitude of the prominence shock. Secondly, we estimate the coronal magnetic field by using some models of prominence coronal seismology, and the results are in agreement with the available data in the literature.
【學(xué)位授予單位】：山東大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P182
【參考文獻】
相關(guān)期刊論文 前1條
1 CHEN Yao;;A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions[J];Chinese Science Bulletin;2013年14期
，本文編號：2258641
本文鏈接：http://sikaile.net/kejilunwen/tianwen/2258641.html
