本文選題：磁繩　切入點(diǎn)：耀斑　出處：《中國科學(xué)技術(shù)大學(xué)》2017年博士論文　論文類型：學(xué)位論文

【摘要】：耀斑和日冕物質(zhì)拋射(CME)是發(fā)生在太陽上常見的劇烈活動,作為空間天氣擾動的主要驅(qū)動源,深刻的影響著地球上人類的生活和科技。耀斑與CME常常呈現(xiàn)伴生關(guān)系,有著強(qiáng)的關(guān)聯(lián)。耀斑作為太陽局地現(xiàn)象,觀測上為非常寬廣的輻射譜增強(qiáng)信息;CME作為傳播結(jié)構(gòu),除了遙感觀測,還有對其內(nèi)部粒子和磁場的觀測。本文從分析觀測資料出發(fā),探討CME初始階段的形態(tài)和觸發(fā)機(jī)制,構(gòu)建極紫外(EUV)熱力學(xué)圖譜分析耀斑的輻射過程。1,構(gòu)建極紫外熱力學(xué)圖譜分析耀斑的輻射過程:SDO上搭載的EVE(極紫外成像儀,EUV Variability Experiment)提供太陽活動的豐富的熱力學(xué)過程,特別是對于太陽耀斑。基于EVE譜線我們構(gòu)建了熱力學(xué)圖譜(TDS thermodynamic spectrum),這種工具將來也可應(yīng)用于研究遙遠(yuǎn)星體的爆發(fā)活動。通過對研究幾個事例,我們展示TDS圖譜的功能。更進(jìn)一步,我們將TDS方法應(yīng)用于74個大于M5.0的耀斑分析,并且得到了如下統(tǒng)計結(jié)論:1,EUV的峰值總是滯后于軟X射線(SXR)的峰值,同時越強(qiáng)的耀斑其冷卻率越快。峰值的延遲時間和冷卻率存在冪律關(guān)系,表征了合乎邏輯的從SXR到EUV的冷卻輻射過程;2,耀斑熱力學(xué)圖譜呈現(xiàn)出兩種截然不同的溫度漂移模式,Ⅰ型和Ⅱ型。Ⅰ型耀斑,從高溫到低溫增強(qiáng)的輻射漂移部分像個四邊形,而Ⅱ型耀斑的漂移部分則像個三角形。統(tǒng)計分析認(rèn)為,相較于Ⅰ型,Ⅱ型耀斑更為脈沖;3,對于存在后相的耀斑,后相的峰值強(qiáng)度與主相峰值強(qiáng)度的比率粗略上正相關(guān)于耀斑等級,且強(qiáng)后相的耀斑都是束縛事件。我們相信,TDS圖譜顯示,對于束縛事件,未能成功爆發(fā)的磁繩所攜帶的能量激發(fā)了熱輻射過程。TDS圖譜同時還展示了色球?qū)雍瓦^渡區(qū)的熱力學(xué)過程。這些結(jié)果對于提高我們認(rèn)知耀斑和相關(guān)爆發(fā)(CME)提供了新的線索和方法。2,研究了 CME爆發(fā)前的磁繩形態(tài)以及爆發(fā)過程中的運(yùn)動過程:CME的磁繩結(jié)構(gòu)最早是基于當(dāng)?shù)靥栵L(fēng)的磁云觀測得到的,回溯到低日冕,由于沒有直接的日冕磁場觀測,磁繩是否存在于CME拋射之前在各種CME理論和數(shù)值模型下眾說紛紜。為了探究CME初始形態(tài)以及耀斑期間其動力學(xué)過程,我們研究2011年6月21日的C7.7級的超長持續(xù)時間的耀斑,它在GOES(近地同步環(huán)境監(jiān)測衛(wèi)星,Geostationary Operational Environment Satellite)軟 X 射線通量觀測曲線上表現(xiàn)為兩個小時的通量上升,而對于一個典型的耀斑,上升相的持續(xù)時間不過數(shù)十分鐘甚至短短幾分鐘。在SDO(太陽動力學(xué)觀測臺,Solar Dynamic Observatory)的視角下,該耀斑處于日面中央,而在STEREO(日地關(guān)系觀測臺,Solar TErrestrialRElations Observatory)雙星的視角下,該耀斑位置處于日面邊緣,由此,第一次重構(gòu)出了爆發(fā)前活動區(qū)S型整體三維結(jié)構(gòu),利用AIA(太陽大氣成像儀,Atmospheric Imaging Assembly)的極紫外高溫譜線(94A,131A)展示了此結(jié)構(gòu)在爆發(fā)前的局部活動和形態(tài)以及爆發(fā)過程中的動力學(xué)過程。這種S型結(jié)構(gòu)常被直接解釋為磁繩本體,在爆發(fā)前平均高度達(dá)到了60Mm。在初始階段,磁繩西側(cè)肘部的磁靜力學(xué)平衡被破壞驅(qū)動了爆發(fā)前相,導(dǎo)致磁繩結(jié)構(gòu)的緩慢上升,隨后的底部磁重聯(lián)和(或)磁繩不穩(wěn)定性導(dǎo)致了爆發(fā)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.

【學(xué)位授予單位】：中國科學(xué)技術(shù)大學(xué)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2017
【分類號】：P182.62

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本文編號：1616173