使用SDO / AIA觀測閃焰亮帶之運動情形

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姓名

楊昀蓁(Yun-Chen Yang) 查詢紙本館藏

畢業系所

太空科學研究所

論文名稱

使用SDO / AIA觀測閃焰亮帶之運動情形
(Elongation and Separation of Flare Ribbons by Using SDO/AIA)

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摘要(中)

紫外線波段所觀察到的閃焰亮帶結構，可能是由於閃焰環頂磁場重構區域的加速粒子撞擊至低層大氣而產生，也可能與熱傳導效應有關。二維標準閃焰模型雖然可以定性解釋磁場重構所造成的成對亮帶相對於磁極反轉線彼此遠離的現象，但觀測上明顯能看到閃焰亮區也有沿著磁極反轉線方向上的變化。為了探討此一現象，本篇論文使用SDO/AIA 1600 A影像分析2011年2月到2014年12月間的46起閃焰事件，將累計亮度圖中的最大梯度處視為亮帶邊緣，藉以估算亮帶兩端點的延展運動及亮帶最外緣的分離運動情形，發現在閃焰的主要能量釋放階段，亮帶的平均延展速率(約56 km/s)大於分離速率(約26 km/s)。並根據磁極反轉線兩側的亮帶延展方向將事件分成三類：(1)兩側亮帶主要延展方向相同，共18起事件，(2)兩側亮帶延展方向相反，共23起事件，(3)只有一側亮帶有明顯延展運動的事件有5起。我們的研究結果顯示，此三類的亮帶延展速率與F ?_SXR和????????的峰值及???????? fluence並沒有很好的相關性，但發現較大的閃焰似乎較好發於亮帶延展方向相反的事件，其背後的物理意義有待將來再詳加仔細研究。

摘要(英)

The flare ribbon structure seen in ultraviolet images can be either caused by the flare-accelerated particles impacting on the lower solar atmosphere or related to the thermal conduction. Besides the separation between two ribbons expected by the CSHKP model, the elongation of flare ribbons along the magnetic polarity inversion line is also observed. In order to figure out the possible causes of ribbon elongation, we used the SDO/AIA 1600 A data in this study to analyze 46 selected flare events from 2011 February to 2014 December. The maximum gradient of brightening in a stack-plot is taken as the outermost boundary of a flare ribbon for speed estimations. We found that in the impulsive phase, the averaged elongation speed (~56 km/s) is larger than the averaged separation speed (~26 km/s). In addition, the elongation motion can be classified into three groups, namely, the same direction between two ribbons (18 events in total), the opposite directions (23 events in total) between two ribbons, and the motion only seen in one side of flare ribbons (5 events in total). There is no apparent correlation between the elongation speed and the peak of F ?_SXR and F_SXR, and the F_SXR fluence. But those flares with the larger F_SXR peak or the larger F_SXR fluence are likely to be associated with the opposite elongation, which can be studied more detailed in a future.

關鍵字(中)

★ 太陽
★ 閃焰
★ 亮帶

關鍵字(英)

★ solar
★ flare
★ ribbon

論文目次

中文摘要 i
英文摘要 ii
致謝 iii
目錄 iv
圖目錄 vi
表目錄 viii
第一章緒論 1
1.1 太陽閃焰 1
1.2 二維標準閃焰模型 4
1.3 相關文獻回顧 10
1.4 F_SXR 與 F_HXR 14
1.5 研究動機 17
第二章方法與資料 18
2.1 觀測儀器與資料 18
2.1.1 AIA 18
2.1.2 HMI 21
2.2 資料選取來源 23
2.3 累計圖 (stack-plot) 24
2.4 速率的估算 29
第三章資料分析與結果 30
3.1 平行方向的亮帶延展 31
3.1.1 同向 31
3.1.2 反向 36
3.1.3 單側延展 40
3.2 垂直方向的分離運動 44
3.3 二次爆發的事件 47
3.4 總結 49
第四章討論 52
4.1 造成磁場重構之可能原因 52
4.2 磁場重構區域之能量釋放 58
4.3 線性磁流體波傳遞擾動 64
第五章結論 65
參考文獻 67

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指導教授

楊雅惠(Ya-Hui Yang)

審核日期

2018-7-27

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