太阳日珥震荡的观测和理论研究
发布时间：2018-10-09 08:21
【摘要】：太阳日珥震荡常涉及多方面的太阳活动,包括活动区爆发(主要是耀斑和CME)及其所触发的日冕波动传播,以及引起邻近日珥结构震荡的主要扰动EUV波。我们所研究的三列日珥震荡事件是由同一日珥结构在受到邻近活动区爆发事件的作用下发生的,这一日珥结构在序列扰动下的不同震荡表现为研究有关物理机制提供了很好的机会。此外,对日珥震荡参数的观测分析已经成为日珥冕震学测量磁场的一个重要手段。因此,对日珥震荡的研究具有非常重要的科学意义。本文利用SDO/AIA的观测数据,分析了这三列日珥震荡的产生以及运动特征,主要的内容及结论如下：我们首先分析了震荡驱动源—活动区处发生的相应耀斑和CME事件,三次爆发都观测到了M级的耀斑,其中后两次爆发也伴随有CME。在差分图上可以观测到后两次CME驱动的EUV波前沿,根据CME爆发和日珥震荡起始的时间差,我们计算了EUV波的传播速度,并且确认EUV波是引起日珥震荡的直接原因。对于第一次爆发在差分图上没有看到EUV波前沿,然而结合日冕波动传播速度v=967±50 Km/s,我们猜测这列波动有可能对应于耀斑驱动的莫尔顿波(Morten wave)或爆震波(blast wave).随后我们对同一震荡不同高度的日珥做切片,得到震荡波形并且测量了它们的起始时间和周期振幅等参数。最后对三列日珥震荡进行比较,确认它们的震荡模式是集体kink震荡。此外,我们还研究了horn的震荡行为,同日珥震荡做了比较,发现二者在周期振幅等参数上有很多不同,我们认为这是由于horn延伸入冕腔中,受到大尺度日冕磁场结构的影响,因而表现出与日珥震荡不同的观测特征,据我们所知,这是首次报道的horn准周期震荡现象。另外,我们对日珥震荡的参数进行了拟合,主要是应用一个衰减的正弦函数加上一个线性的漂移函数,分别得到了三列震荡的周期为25±2 min,36±2 min,28±2 min,振幅为2.62±1.0 arcsec,8.59±1.0 arcsec,9.07±1.0 arcsec和衰减时间120±20 min,145±20 min,165±10min,通过衰减时间,简单的分析了日珥震荡的衰减机制,同时计算了震荡初始速度幅度,说明了这三列震荡都是较大幅度的日珥震荡。其次,我们利用日珥冕震学的一些模型估算了日冕磁场,所得结果与文献中的已有数据相符。
[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 卤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 卤2 min,36 卤2 min,28 卤2 min, the amplitude is 2. 62 卤1. 0 arcsec,8.59 卤1. 0 arcsec,9.07 卤1. 0 arcsec and the attenuation time is 120 卤20 min,145 卤20 min,165 卤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.
【学位授予单位】：山东大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P182
本文编号：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 卤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 卤2 min,36 卤2 min,28 卤2 min, the amplitude is 2. 62 卤1. 0 arcsec,8.59 卤1. 0 arcsec,9.07 卤1. 0 arcsec and the attenuation time is 120 卤20 min,145 卤20 min,165 卤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.
【学位授予单位】：山东大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P182
【参考文献】
相关期刊论文 前1条
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
，本文编号：2258641
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