太阳大气三维磁场结构及相关活动现象的研究
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摘要
太阳大气由高度磁化的等离子体组成,磁场对理解太阳大气中的各种活动现象(比如耀斑、暗条、日珥以及日冕物质抛射)起着至关重要的作用。近几年来发展的一系列非线性无力场外推的方法以及由先进的光谱偏振计得到的矢量磁场为太阳磁场本身以及相关的活动现象研究提供了一个全新的视角。本论文针对太阳活动区及活动现象进行了深入的观测和无力场建模研究。首先,我们对偏振观测及磁场反演的有效性进行了探讨。其次,我们对活动区和暗条的三维磁场结构进行了详细的分析。我们系统地阐述了偏振光谱的观测、从斯托克斯参数到磁场的反演、矢量磁场的分析和太阳三维磁场的外推,在此基础上进一步分析了耀斑、暗条以及日冕物质抛射等活动现象的机制及其相互联系,得到了如下所述的新的结果。
我们使用基于米尔恩-爱丁顿(Milne-Eddington)太阳大气模型的两个磁场反演程序构造和比较了两个光谱偏振计得到的矢量磁图,其中一个是地面望远镜THEMIS上的多谱线偏振光谱仪(MTR),另外一个是空间望远镜日出(Hinode)卫星上的光学望远镜分光偏振计(SOT/SP)。为此,我们分析了2008年5月23日NOAA10996活动区内一个光斑区域的观测。就磁场强度、方位角以及磁场倾角的分布而言,我们发现不同的磁场反演程序和仪器观测给出的结果是一致的。因为日出卫星的分光偏振计不受视宁度问题的影响,我们能够分辨出具有1“到2”尺寸的磁极,并且能够探测到在负极和正极区域分别汇聚和散开的水平磁场。这些发现支持光斑是由小的磁流管束组成的。我们提出了一个新的方法来得到多条谱线的相对形成高度,并且发现FeⅠ6302.5?谱线比FeⅠ5250.2?谱线形成在更高的大气高度。
我们研究了2006年12月13日双带耀斑的三维磁场位形,特别是使用优化的方法来构造非线性无力场模型。外推所需的高空间分辨率的NOAA10930活动区的光球矢量磁场观测由日出卫星上的分光偏振计得到。磁场的拓扑结构可以描述为一个高度剪切的核区磁场加上一个接近势场的包层拱状磁场。核区磁场清楚地显示出一些用来支撑暗条的磁凹陷结构。由非线性无力场所包含的能量减去对应的势场能量,计算出的耀斑释放的自由能大约是2.4×1031尔格,这个能量大约是耀斑前势场能量的2%。我们还计算了剪切角,即非线性无力场和势场的夹角。我们发现耀斑后剪切角在低层大气的某些位置变得更大,而在大部分的位置它们明显变小,这表明整个磁场位形在耀斑后变得更接近势场。太阳光学望远镜的宽带滤光成像仪(BFI)得到的Ca II H谱线图像和紫外的1600A图像显示耀斑前的加热主要发生在核区磁场。这些结果提供了支持太阳耀斑缰绳断裂(tether-cutting)模型的证据。我们还使用日出卫星上的极紫外成像分光计(EIS)观测研究了活动区内极紫外谱线的形成高度。在使用双高斯拟合解决了He II 256.32 A和Si x 256.37 A谱线的混合问题之后,通过比较日面上的多普勒分布和磁场分布,我们发现过渡区在强磁场的区域会升高,在耀斑前加热的区域可能存在多种温度的环结构。
使用非线性无力场外推的方法,我们还研究了NOAA10767活动区暗条的磁场位形。光球的矢量磁场通过THEMIS的多谱线偏振光谱仪在2005年5月27日观测得到。我们提出了一个新的去除横场180°不确定性的方法。通过使观测矢量磁场的总磁力和总力矩最小化来对观测数据进行预处理,这一步为非线性无力场模型提供了一致的底边界条件。然后,我们使用优化的方法计算了日冕的磁场,从而找到了一个沿着磁场极性反转线的磁通量绳。这个磁通量绳和一个Hα暗条的一部分在空间上对应得非常好,而整个磁凹陷的分布则对应了整个Hα暗条。这意味着这个暗条磁场结构的一部分是磁绳,而另外一部分是剪切的磁拱。磁拱在负螺度的磁场里诱生了一个左生的暗条,这和一个磁绳在相同螺度的磁场里诱生的暗条分叉的手性是相反的。暗条中心的磁场强度大约是700高斯。在同一个活动区里发生了一个M1.1级的耀斑。磁绳或者说暗条爆发的紫外观测显示出爆发结构有一个很强的扭曲运动,这表明在爆发过程中磁绳把它的部分缠绕转化成了磁绳中心轴的扭曲。在计算了爆发前磁绳的缠绕数以后,我们发现它和一些数值模拟得到的螺旋扭曲不稳定性(helical kink instability)的临界值符合得非常好。我们推断出磁绳的激活和初始阶段的上升由扭曲不稳定性触发和驱动。我们还使用势场模型估计了爆发前外部磁场衰减指数随着高度的分布。衰减指数在爆发磁绳之上的很大一个高度范围之内都保持低于螺线环不稳定性(torus instability)发生的阈值。这就为这个失败的爆发提供了一个可能的解释。
我们进一步研究了与各种太阳活动现象有关的磁场拓扑和螺度注入。首先,我们发现磁场零点和日冕亮点有着紧密的关系。一个磁零点的线性结构由脊线和扇面来描述。脊线和扇面处的磁场重联产生了日冕亮点。其次,磁场零点并不是在所有的磁活动中都出现。通过研究与2005年5月27日M1.1级耀斑相联系的准分界面,发现紫外线显示的耀斑带和准分界面与光球的交界面在空间上对应得很好。这个M1.1级耀斑峰值时刻的硬X射线源对应于爆发螺旋结构的足点,这表明磁绳内部可以有效地产生硬X射线源。最后,我们研究了磁绳缠绕数的演化和磁螺度注入的关系,发现它们之间有着近似线性的正相关关系。不论是水平方向运动(比如旋转和剪切)还是竖直方向运动(比如磁通量浮现)都可以增加缠绕数,然后引起磁绳的爆发,从而导致日冕物质抛射的形成。
The solar atmosphere is constituted of highly magnetized plasma. Magnetic fields play a key role in understanding various active phenomena in the solar atmosphere, such as flares, filaments and prominences, and coronal mass ejections. Various nonlin-ear force-free field extrapolation methods developed in the past years and vector mag-netic fields obtained by sophisticated spectro-polarimeters provide a totally new view on the solar magnetic fields and associated activities and phenomena. In this thesis, we perform a detailed study on the solar active regions and active phenomena via obser-vations and force-free field modelling. First, we discuss the polarization observation and the validity of magnetic field inversion codes. Then, we analyze in detail the three dimensional magnetic field structure of active regions and filaments. We systemati-cally discuss the observation of polarization profiles, the Stokes inversion of magnetic fields, the analysis of vector magnetic fields in the photosphere, and extrapolations of magnetic fields to upper layers. Based on these, we further analyze the mechanisms of solar flares, filaments/prominences, and coronal mass ejections, and the relationships between them. Finally, we obtain the new results as follows.
Using the two inversion codes (UNNOFIT and MELANIE) based on the Milne-Eddington solar atmospheric model, we build and compare vector magnetic maps obtained by two spectro-polarimeters, of which one is the ground-based Telescope Heliographique pour l'Etude du Magnetisme et des Instabilites Solaires/Multi-Raies (THEMIS/MTR) and the other is Solar Optical Telescope/Spectro-Polarimeter (SOT/SP) on board Hinode. To this end, we adopt the observation of a facular region within the active region NOAA 10996 on 2008 May 23, and find consistent results concerning the field strength, azimuth, and inclination distributions. Because SOT/SP is free from the seeing effect and has better spatial resolution, we are able to resolve small magnetic polarities with sizes of 1" to 2", and we can detect strong horizontal magnetic fields, which converge or diverge in negative or positive facular polarities. These findings support models which suggest the existence of small vertical flux tube bundles in faculae. A new method is proposed to get the relative formation heights of the multi-lines observed by MTR assuming the validity of a flux tube model for the faculae. We found that the FeⅠ6302.5 A line is formed higher than the FeⅠ5250.2 A line.
We study the three-dimensional magnetic field configuration of the two-ribbon flare in the active region NOAA 10930 on 2006 December 13, using the optimization method for nonlinear force-free field (NLFFF) extrapolation and the photospheric vector mag-netic field with high spatial resolution obtained by Hinode SOT/SP. The magnetic topol-ogy can be described as a highly sheared core field and a quasi-potential envelope field of magnetic arcades. The core field clearly shows some dips supposed to sustain a fila-ment. Free energy release in the flare, calculated by subtracting the energy contained in the NLFFF and the corresponding potential field, is 2.4×1031 ergs, which is about 2% of the energy in the potential field before the flare. We also calculate the shear angles, defined as the angles between the NLFFF and potential fields, and find that they be-come larger at some particular sites in the lower atmosphere after the flare, while they become significantly smaller in most places implying that the whole configuration gets closer to the potential field. The CaⅡH line images obtained with the Broadband Filter Imager (BFI) of the SOT and the 1600 A images with the Transition Region and Coro-nal Explorer(TRACE) show that the pre-flare heating occurs mainly in the core field. These results provide evidence in support of the tether-cutting model of solar flares. In addition, we study the correlation heights, which indicate the formation height of Extreme Ultraviolet (EUV) lines in the active region using observations from the EUV Imaging Spectrometer (EIS) on board Hinode. After solving the line blending problem between the HeⅡ256.32 A and SiⅩ256.37 A lines by the double Gaussian curve fitting, we find that the transition region lies higher in a strong magnetic area. In a pre-flare heating area, there possibly exist multi-thermal loops as implied by comparing the Doppler velocity and the magnetic field on the solar disk.
We compute the three-dimensional magnetic field of the active region NOAA 10767 in order to study the magnetic configuration of active region filaments. The NLFFF model is adopted to compute the magnetic field above the photosphere, where the vector magnetic field was observed by THEMIS/MTR on 2005 May 27. We propose a new method to remove the 180°ambiguity of the transverse field. We then analyze the implications of the preprocessing of the data by minimizing the total force and torque in the observed vector fields. This provides a consistent bottom boundary condition for the NLFFF model. Then, using the optimization method to compute the coronal field, we find a magnetic flux rope along the polarity inversion line. The magnetic flux rope aligns well with part of an Ha filament, while the total distribution of the magnetic dips coincides with the whole Ha filament. This implies that the magnetic field structure in one section of the filament is a flux rope, while the other is a sheared arcade. The arcade induced a left-bearing filament in the magnetic field of negative helicity, which is opposite to the chirality of barbs that a flux rope, having a magnetic field of the same helicity sign, would induce. The field strength in the center of the flux rope is about 700 Gauss. An M1.1 flare occurred in the same active region. TRACE observations of the flux rope or filament eruption show a strong writhing motion of the erupting structure, suggesting that the flux rope converted some of its twist into writhe during the eruption. After calculating the twist of the pre-eruptive flux rope, we find that it is in very good agreement with thresholds of the helical kink instability found in numerical simulations. We conclude that the activation and rise of the flux rope were triggered and initially driven by the kink instability. We also estimate the height distribution of the decay index of the external magnetic field before the eruption with a potential field. The decay indices stay below the threshold for the "torus instability" for a significant height range above the erupting flux rope. This provides a possible explanation for the confinement of the eruption, hence for the absence of a CME.
With three-dimensional magnetic fields, we further study the magnetic topology and helicity injection associated with different solar activities. First, we find that magnetic null points have a close relationship with coronal bright points. The linear structure of a null point is described by the spine and fan. Magnetic reconnection in the spine and fan produces coronal bright points. Second, since magnetic null points are not necessarily present in all regions, we study the quasi-separatrix layer (QSL) associated with the M1.1 flare on 2005 May 27, and find that the ultraviolet flare ribbon of the flare coincides well with the intersection between the QSL and the photosphere, while hard X-ray (HXR) sources at the peak of the flare seem to coincide with the foot-points of the erupting helical structures, which indicates a high possibility that HXR sources can be produced efficiently in the flux rope. Finally, the relationship between the evolution of the twist of a flux rope and the helicity injection is studied. They have a positive relationship with each other. Helicity injection by both horizontal motions, such as twisting and shearing, and vertical motions, such as flux emergence, could increase the twist and cause an eruption of a flux rope, which leads to the formation of CMEs.
我们使用基于米尔恩-爱丁顿(Milne-Eddington)太阳大气模型的两个磁场反演程序构造和比较了两个光谱偏振计得到的矢量磁图,其中一个是地面望远镜THEMIS上的多谱线偏振光谱仪(MTR),另外一个是空间望远镜日出(Hinode)卫星上的光学望远镜分光偏振计(SOT/SP)。为此,我们分析了2008年5月23日NOAA10996活动区内一个光斑区域的观测。就磁场强度、方位角以及磁场倾角的分布而言,我们发现不同的磁场反演程序和仪器观测给出的结果是一致的。因为日出卫星的分光偏振计不受视宁度问题的影响,我们能够分辨出具有1“到2”尺寸的磁极,并且能够探测到在负极和正极区域分别汇聚和散开的水平磁场。这些发现支持光斑是由小的磁流管束组成的。我们提出了一个新的方法来得到多条谱线的相对形成高度,并且发现FeⅠ6302.5?谱线比FeⅠ5250.2?谱线形成在更高的大气高度。
我们研究了2006年12月13日双带耀斑的三维磁场位形,特别是使用优化的方法来构造非线性无力场模型。外推所需的高空间分辨率的NOAA10930活动区的光球矢量磁场观测由日出卫星上的分光偏振计得到。磁场的拓扑结构可以描述为一个高度剪切的核区磁场加上一个接近势场的包层拱状磁场。核区磁场清楚地显示出一些用来支撑暗条的磁凹陷结构。由非线性无力场所包含的能量减去对应的势场能量,计算出的耀斑释放的自由能大约是2.4×1031尔格,这个能量大约是耀斑前势场能量的2%。我们还计算了剪切角,即非线性无力场和势场的夹角。我们发现耀斑后剪切角在低层大气的某些位置变得更大,而在大部分的位置它们明显变小,这表明整个磁场位形在耀斑后变得更接近势场。太阳光学望远镜的宽带滤光成像仪(BFI)得到的Ca II H谱线图像和紫外的1600A图像显示耀斑前的加热主要发生在核区磁场。这些结果提供了支持太阳耀斑缰绳断裂(tether-cutting)模型的证据。我们还使用日出卫星上的极紫外成像分光计(EIS)观测研究了活动区内极紫外谱线的形成高度。在使用双高斯拟合解决了He II 256.32 A和Si x 256.37 A谱线的混合问题之后,通过比较日面上的多普勒分布和磁场分布,我们发现过渡区在强磁场的区域会升高,在耀斑前加热的区域可能存在多种温度的环结构。
使用非线性无力场外推的方法,我们还研究了NOAA10767活动区暗条的磁场位形。光球的矢量磁场通过THEMIS的多谱线偏振光谱仪在2005年5月27日观测得到。我们提出了一个新的去除横场180°不确定性的方法。通过使观测矢量磁场的总磁力和总力矩最小化来对观测数据进行预处理,这一步为非线性无力场模型提供了一致的底边界条件。然后,我们使用优化的方法计算了日冕的磁场,从而找到了一个沿着磁场极性反转线的磁通量绳。这个磁通量绳和一个Hα暗条的一部分在空间上对应得非常好,而整个磁凹陷的分布则对应了整个Hα暗条。这意味着这个暗条磁场结构的一部分是磁绳,而另外一部分是剪切的磁拱。磁拱在负螺度的磁场里诱生了一个左生的暗条,这和一个磁绳在相同螺度的磁场里诱生的暗条分叉的手性是相反的。暗条中心的磁场强度大约是700高斯。在同一个活动区里发生了一个M1.1级的耀斑。磁绳或者说暗条爆发的紫外观测显示出爆发结构有一个很强的扭曲运动,这表明在爆发过程中磁绳把它的部分缠绕转化成了磁绳中心轴的扭曲。在计算了爆发前磁绳的缠绕数以后,我们发现它和一些数值模拟得到的螺旋扭曲不稳定性(helical kink instability)的临界值符合得非常好。我们推断出磁绳的激活和初始阶段的上升由扭曲不稳定性触发和驱动。我们还使用势场模型估计了爆发前外部磁场衰减指数随着高度的分布。衰减指数在爆发磁绳之上的很大一个高度范围之内都保持低于螺线环不稳定性(torus instability)发生的阈值。这就为这个失败的爆发提供了一个可能的解释。
我们进一步研究了与各种太阳活动现象有关的磁场拓扑和螺度注入。首先,我们发现磁场零点和日冕亮点有着紧密的关系。一个磁零点的线性结构由脊线和扇面来描述。脊线和扇面处的磁场重联产生了日冕亮点。其次,磁场零点并不是在所有的磁活动中都出现。通过研究与2005年5月27日M1.1级耀斑相联系的准分界面,发现紫外线显示的耀斑带和准分界面与光球的交界面在空间上对应得很好。这个M1.1级耀斑峰值时刻的硬X射线源对应于爆发螺旋结构的足点,这表明磁绳内部可以有效地产生硬X射线源。最后,我们研究了磁绳缠绕数的演化和磁螺度注入的关系,发现它们之间有着近似线性的正相关关系。不论是水平方向运动(比如旋转和剪切)还是竖直方向运动(比如磁通量浮现)都可以增加缠绕数,然后引起磁绳的爆发,从而导致日冕物质抛射的形成。
The solar atmosphere is constituted of highly magnetized plasma. Magnetic fields play a key role in understanding various active phenomena in the solar atmosphere, such as flares, filaments and prominences, and coronal mass ejections. Various nonlin-ear force-free field extrapolation methods developed in the past years and vector mag-netic fields obtained by sophisticated spectro-polarimeters provide a totally new view on the solar magnetic fields and associated activities and phenomena. In this thesis, we perform a detailed study on the solar active regions and active phenomena via obser-vations and force-free field modelling. First, we discuss the polarization observation and the validity of magnetic field inversion codes. Then, we analyze in detail the three dimensional magnetic field structure of active regions and filaments. We systemati-cally discuss the observation of polarization profiles, the Stokes inversion of magnetic fields, the analysis of vector magnetic fields in the photosphere, and extrapolations of magnetic fields to upper layers. Based on these, we further analyze the mechanisms of solar flares, filaments/prominences, and coronal mass ejections, and the relationships between them. Finally, we obtain the new results as follows.
Using the two inversion codes (UNNOFIT and MELANIE) based on the Milne-Eddington solar atmospheric model, we build and compare vector magnetic maps obtained by two spectro-polarimeters, of which one is the ground-based Telescope Heliographique pour l'Etude du Magnetisme et des Instabilites Solaires/Multi-Raies (THEMIS/MTR) and the other is Solar Optical Telescope/Spectro-Polarimeter (SOT/SP) on board Hinode. To this end, we adopt the observation of a facular region within the active region NOAA 10996 on 2008 May 23, and find consistent results concerning the field strength, azimuth, and inclination distributions. Because SOT/SP is free from the seeing effect and has better spatial resolution, we are able to resolve small magnetic polarities with sizes of 1" to 2", and we can detect strong horizontal magnetic fields, which converge or diverge in negative or positive facular polarities. These findings support models which suggest the existence of small vertical flux tube bundles in faculae. A new method is proposed to get the relative formation heights of the multi-lines observed by MTR assuming the validity of a flux tube model for the faculae. We found that the FeⅠ6302.5 A line is formed higher than the FeⅠ5250.2 A line.
We study the three-dimensional magnetic field configuration of the two-ribbon flare in the active region NOAA 10930 on 2006 December 13, using the optimization method for nonlinear force-free field (NLFFF) extrapolation and the photospheric vector mag-netic field with high spatial resolution obtained by Hinode SOT/SP. The magnetic topol-ogy can be described as a highly sheared core field and a quasi-potential envelope field of magnetic arcades. The core field clearly shows some dips supposed to sustain a fila-ment. Free energy release in the flare, calculated by subtracting the energy contained in the NLFFF and the corresponding potential field, is 2.4×1031 ergs, which is about 2% of the energy in the potential field before the flare. We also calculate the shear angles, defined as the angles between the NLFFF and potential fields, and find that they be-come larger at some particular sites in the lower atmosphere after the flare, while they become significantly smaller in most places implying that the whole configuration gets closer to the potential field. The CaⅡH line images obtained with the Broadband Filter Imager (BFI) of the SOT and the 1600 A images with the Transition Region and Coro-nal Explorer(TRACE) show that the pre-flare heating occurs mainly in the core field. These results provide evidence in support of the tether-cutting model of solar flares. In addition, we study the correlation heights, which indicate the formation height of Extreme Ultraviolet (EUV) lines in the active region using observations from the EUV Imaging Spectrometer (EIS) on board Hinode. After solving the line blending problem between the HeⅡ256.32 A and SiⅩ256.37 A lines by the double Gaussian curve fitting, we find that the transition region lies higher in a strong magnetic area. In a pre-flare heating area, there possibly exist multi-thermal loops as implied by comparing the Doppler velocity and the magnetic field on the solar disk.
We compute the three-dimensional magnetic field of the active region NOAA 10767 in order to study the magnetic configuration of active region filaments. The NLFFF model is adopted to compute the magnetic field above the photosphere, where the vector magnetic field was observed by THEMIS/MTR on 2005 May 27. We propose a new method to remove the 180°ambiguity of the transverse field. We then analyze the implications of the preprocessing of the data by minimizing the total force and torque in the observed vector fields. This provides a consistent bottom boundary condition for the NLFFF model. Then, using the optimization method to compute the coronal field, we find a magnetic flux rope along the polarity inversion line. The magnetic flux rope aligns well with part of an Ha filament, while the total distribution of the magnetic dips coincides with the whole Ha filament. This implies that the magnetic field structure in one section of the filament is a flux rope, while the other is a sheared arcade. The arcade induced a left-bearing filament in the magnetic field of negative helicity, which is opposite to the chirality of barbs that a flux rope, having a magnetic field of the same helicity sign, would induce. The field strength in the center of the flux rope is about 700 Gauss. An M1.1 flare occurred in the same active region. TRACE observations of the flux rope or filament eruption show a strong writhing motion of the erupting structure, suggesting that the flux rope converted some of its twist into writhe during the eruption. After calculating the twist of the pre-eruptive flux rope, we find that it is in very good agreement with thresholds of the helical kink instability found in numerical simulations. We conclude that the activation and rise of the flux rope were triggered and initially driven by the kink instability. We also estimate the height distribution of the decay index of the external magnetic field before the eruption with a potential field. The decay indices stay below the threshold for the "torus instability" for a significant height range above the erupting flux rope. This provides a possible explanation for the confinement of the eruption, hence for the absence of a CME.
With three-dimensional magnetic fields, we further study the magnetic topology and helicity injection associated with different solar activities. First, we find that magnetic null points have a close relationship with coronal bright points. The linear structure of a null point is described by the spine and fan. Magnetic reconnection in the spine and fan produces coronal bright points. Second, since magnetic null points are not necessarily present in all regions, we study the quasi-separatrix layer (QSL) associated with the M1.1 flare on 2005 May 27, and find that the ultraviolet flare ribbon of the flare coincides well with the intersection between the QSL and the photosphere, while hard X-ray (HXR) sources at the peak of the flare seem to coincide with the foot-points of the erupting helical structures, which indicates a high possibility that HXR sources can be produced efficiently in the flux rope. Finally, the relationship between the evolution of the twist of a flux rope and the helicity injection is studied. They have a positive relationship with each other. Helicity injection by both horizontal motions, such as twisting and shearing, and vertical motions, such as flux emergence, could increase the twist and cause an eruption of a flux rope, which leads to the formation of CMEs.
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