日珥精细结构的IRIS卫星紫外光谱观测研究
发布时间：2018-11-04 14:14
【摘要】：日珥是太阳大气中的重要特征物,其形成与演化一直是太阳物理研究的重要课题。日珥的形态各异,其拓扑形状与日珥磁场位形及其形成机制有密切关系。日珥通常是由精细的细丝状等离子体结构组成的。这些细丝结构体现了日珥的磁场位形,因此是我们认识日珥磁场位形的重要途径。IRIS卫星的成像和光谱观测具有很高的空间和时间分辨率,为我们研究日珥的精细结构提供极佳的手段。本研究工作主要利用IRIS卫星的成像和光谱仪器,分析细丝状结构、垂向流动和小尺度等离子体团等日珥精细结构的几何信息和等离子体流动信息。在这个工作中,我们分析了两个宁静区日珥和一个中间区日珥。我们发现,在IRIS的数据分辨率下,细丝的宽度为0.5"-1",与之前Hα以及SOT Ca Ⅱ的观测结果相同。结合成像和光谱数据我们辨认了这些日珥中数条精细细丝结构,它们在成像观测中均表现为垂直于日面,即以往定义下的垂直细丝。通过分析它们的成像和光谱观测数据,我们得到不同的细丝的天空平面速度分布在10km/s-45km/s之间,多普勒速度分布在10km/s-49km/s之间。结合多普勒速度和天空平面速度,我们推测出了这些细丝与太阳表面在视线方向上的实际夹角。我们发现所谓的'垂直'细丝并不与太阳表面真的垂直,它们与太阳表面的夹角在30°-60°之间,与垂角偏离较大。通过分析细丝内各个位置与太阳表面的夹角,我们发现细丝并不是直的,而是弯曲的,细丝具有类似波浪状结构。垂直细丝与水平细丝的拓扑形状相似,垂直细丝和水平细丝的区别有可能是相对日珥的观测角度导致的。我们认为,这些波浪形磁场拓扑提供了向上的磁张力,可以为日珥等离子体提供支撑。另一方面,在同一日珥中,通过光谱学诊断和成像跟踪观测,我们证实了日珥中存在方向相反的等离子体流动,证明了日珥内部等离子动力学的复杂性。我们在宁静区日珥中发现了两类可能的日珥物质流失的运动形式。一种是等离子体沿磁力线回落太阳表面;另外一种是从日珥无规则脱落的小尺度等离子体团。在其中一个宁静区日珥的演化过程中,我们观察到等离子体团从一侧上升,在另外一侧回落,且其中存在向上运动的气泡结构,整个演化过程,与日珥的磁热对流形成机制相符。通过对这些精细结构的研究,我们对日珥的几何结构、磁场位形和其中的磁流体力学特征有了深入的认识,为将来进一步利用多波段成像和光谱观测研究日珥演化的物理过程提供了重要的线索。
[Abstract]:Prominence is an important characteristic of the solar atmosphere, its formation and evolution has been an important subject in the study of solar physics. The shape of prominence is different, and its topological shape is closely related to the configuration of magnetic field of prominence and its formation mechanism. Prominence usually consists of fine filamentous plasma structures. These filaments reflect the magnetic field configuration of prominence, so it is an important way to understand the magnetic field configuration of prominence. The imaging and spectral observation of IRIS satellite have high spatial and temporal resolution. It is an excellent tool for us to study the fine structure of prominence. In this work, the geometric information and plasma flow information of fine structures such as filaments, vertical flow and small scale plasma clusters are analyzed by IRIS satellite imaging and spectrometer. In this work, we analyzed two quiet areas of prominence and an intermediate region of prominence. We find that the width of filaments is 0.5 "-1" at the resolution of IRIS data, which is the same as that of H 伪 and SOT Ca 鈪，
本文编号：2310059
[Abstract]:Prominence is an important characteristic of the solar atmosphere, its formation and evolution has been an important subject in the study of solar physics. The shape of prominence is different, and its topological shape is closely related to the configuration of magnetic field of prominence and its formation mechanism. Prominence usually consists of fine filamentous plasma structures. These filaments reflect the magnetic field configuration of prominence, so it is an important way to understand the magnetic field configuration of prominence. The imaging and spectral observation of IRIS satellite have high spatial and temporal resolution. It is an excellent tool for us to study the fine structure of prominence. In this work, the geometric information and plasma flow information of fine structures such as filaments, vertical flow and small scale plasma clusters are analyzed by IRIS satellite imaging and spectrometer. In this work, we analyzed two quiet areas of prominence and an intermediate region of prominence. We find that the width of filaments is 0.5 "-1" at the resolution of IRIS data, which is the same as that of H 伪 and SOT Ca 鈪，
本文编号：2310059
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