日冕结构在爆发过程中的温度漂移及动力学演化

发布时间:2018-03-15 16:51

  本文选题:磁绳 切入点:耀斑 出处:《中国科学技术大学》2017年博士论文 论文类型:学位论文


【摘要】:耀斑和日冕物质抛射(CME)是发生在太阳上常见的剧烈活动,作为空间天气扰动的主要驱动源,深刻的影响着地球上人类的生活和科技。耀斑与CME常常呈现伴生关系,有着强的关联。耀斑作为太阳局地现象,观测上为非常宽广的辐射谱增强信息;CME作为传播结构,除了遥感观测,还有对其内部粒子和磁场的观测。本文从分析观测资料出发,探讨CME初始阶段的形态和触发机制,构建极紫外(EUV)热力学图谱分析耀斑的辐射过程。1,构建极紫外热力学图谱分析耀斑的辐射过程:SDO上搭载的EVE(极紫外成像仪,EUV Variability Experiment)提供太阳活动的丰富的热力学过程,特别是对于太阳耀斑。基于EVE谱线我们构建了热力学图谱(TDS thermodynamic spectrum),这种工具将来也可应用于研究遥远星体的爆发活动。通过对研究几个事例,我们展示TDS图谱的功能。更进一步,我们将TDS方法应用于74个大于M5.0的耀斑分析,并且得到了如下统计结论:1,EUV的峰值总是滞后于软X射线(SXR)的峰值,同时越强的耀斑其冷却率越快。峰值的延迟时间和冷却率存在幂律关系,表征了合乎逻辑的从SXR到EUV的冷却辐射过程;2,耀斑热力学图谱呈现出两种截然不同的温度漂移模式,Ⅰ型和Ⅱ型。Ⅰ型耀斑,从高温到低温增强的辐射漂移部分像个四边形,而Ⅱ型耀斑的漂移部分则像个三角形。统计分析认为,相较于Ⅰ型,Ⅱ型耀斑更为脉冲;3,对于存在后相的耀斑,后相的峰值强度与主相峰值强度的比率粗略上正相关于耀斑等级,且强后相的耀斑都是束缚事件。我们相信,TDS图谱显示,对于束缚事件,未能成功爆发的磁绳所携带的能量激发了热辐射过程。TDS图谱同时还展示了色球层和过渡区的热力学过程。这些结果对于提高我们认知耀斑和相关爆发(CME)提供了新的线索和方法。2,研究了 CME爆发前的磁绳形态以及爆发过程中的运动过程:CME的磁绳结构最早是基于当地太阳风的磁云观测得到的,回溯到低日冕,由于没有直接的日冕磁场观测,磁绳是否存在于CME抛射之前在各种CME理论和数值模型下众说纷纭。为了探究CME初始形态以及耀斑期间其动力学过程,我们研究2011年6月21日的C7.7级的超长持续时间的耀斑,它在GOES(近地同步环境监测卫星,Geostationary Operational Environment Satellite)软 X 射线通量观测曲线上表现为两个小时的通量上升,而对于一个典型的耀斑,上升相的持续时间不过数十分钟甚至短短几分钟。在SDO(太阳动力学观测台,Solar Dynamic Observatory)的视角下,该耀斑处于日面中央,而在STEREO(日地关系观测台,Solar TErrestrialRElations Observatory)双星的视角下,该耀斑位置处于日面边缘,由此,第一次重构出了爆发前活动区S型整体三维结构,利用AIA(太阳大气成像仪,Atmospheric Imaging Assembly)的极紫外高温谱线(94A,131A)展示了此结构在爆发前的局部活动和形态以及爆发过程中的动力学过程。这种S型结构常被直接解释为磁绳本体,在爆发前平均高度达到了60Mm。在初始阶段,磁绳西侧肘部的磁静力学平衡被破坏驱动了爆发前相,导致磁绳结构的缓慢上升,随后的底部磁重联和(或)磁绳不稳定性导致了爆发相。
[Abstract]:Flares and coronal mass ejections (CME) is a common strenuous activity on the sun, as the main driving source of space weather disturbances, a profound impact on human life and earth science and technology. The CME flares and often appear associated, has a strong correlation. The sun flares as a local phenomenon observed for radiation is the broad spectrum of enhanced information; CME as a communication structure, in addition to remote sensing observations, and the internal particle and magnetic field observations. Based on the analysis of observation data of CME on the initial stage of the form and trigger mechanism, construction of extreme ultraviolet (EUV) thermodynamic map analysis of.1 radiation flares, radiation flare construction analysis extreme ultraviolet thermodynamic pattern: SDO is equipped with EVE (extreme ultraviolet imager, EUV Variability Experiment) provides the rich solar thermodynamic process, especially for solar flares. The spectral line based on EVE We constructed a thermodynamic map (TDS thermodynamic spectrum), this tool will also be applied to study the distant stars. By the example of the outbreak, we show TDS map function. Further, we will analysis the TDS method is applied to 74 more than M5.0 flares, and obtain the following conclusions: 1, statistics the peak of EUV always lags behind the soft X ray (SXR) peak, and the stronger the flare cooling rate faster. The peak delay time and cooling rate of the power law relationship, the logical characterization of radiation from the SXR to the cooling process of EUV; 2, flare thermodynamics presents two different kinds of maps the temperature drift model, type I and type II. Type I flare from high temperature to low temperature enhanced radiation drift like a quadrilateral, and the drift of type II flares like a triangle. The statistic analysis, compared with type I, type II Yao Spot more pulse; 3, for after the phase of the flare, the peak strength and the phase of the peak intensity ratio is roughly a flare grade, and strong phase flares are bound events. We believe that TDS shows that the shackles of the event, the flux rope failed to carry out the activation energy for the thermal radiation process of.TDS map also shows the thermodynamic process of the chromosphere and transition region. These results can improve our cognition and flare outbreak (CME) provides a new clue and method of.2, the effect of magnetic rope shape of CME before the outbreak of the outbreak and movement in the process of magnetic rope structure CME was originally based on local magnetic cloud observations of the solar wind, back to the low corona, because there is no direct observation of the coronal magnetic field, magnetic rope exists in the CME projection before CME in a variety of theoretical and numerical model for the controversial. During the inquiry CME initial form and flare its kinetic process, we study the June 21, 2011 C7.7 ultra long duration flare, it in GOES (near earth synchronous satellites for environmental monitoring, Geostationary Operational Environment Satellite) soft X ray flux curve showed two hours of flux increased, and for a typical flare up the duration of phase only tens of minutes or even a few minutes. At SDO (the Solar Dynamics Observatory, Solar Dynamic Observatory) from the perspective of the flare in Japan and in central, STEREO (solar terrestrial relations Observatory, Solar TErrestrialRElations Observatory) double perspective, the position is on the side edge of the flare, thereby. The first time were reconstructed before the outbreak of the active region S type whole three-dimensional structure, the use of AIA (solar atmosphere imaging instrument, Atmospheric Imaging Assembly) extreme ultraviolet High temperature spectral lines (94A, 131A) show the dynamic process of this structure in local activities and form before the outbreak and the outbreak in the process. The S structure is often interpreted as a direct flux rope in the body, before the outbreak of the average height reached 60Mm. in the initial stage, the magnetic flux rope on the west side of the static balance elbow is destroyed the driver before the outbreak phase, causes the structure of the flux rope rises slowly, at the bottom of magnetic reconnection and the subsequent (or magnetic) rope instability causing outbreaks.

【学位授予单位】:中国科学技术大学
【学位级别】:博士
【学位授予年份】:2017
【分类号】:P182.62

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