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姓名 陳煜(Yu Chen) 查詢紙本館藏 畢業系所 太空科學研究所 論文名稱 IRIS Mg II譜線之太陽閃焰色球加熱現象研究
(Investigation of chromospheric heating in solar flares by IRIS Mg II lines)相關論文 檔案 [Endnote RIS 格式]
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摘要(中) 色球蒸散為伴隨太陽閃焰產生的現象，一般認為閃焰產生的非熱電子撞擊至色球層時，除了會在磁管足部附近輻射出硬X射線之外，過程中也會加熱周遭的電漿，造成局部區域的熱電漿沿著磁場向下運動並有接續的色球蒸散發生。因此利用對應於色球層電漿的IRIS Mg II譜線資料，結合GOES軟X射線與RHESSI硬X射線光變曲線，將能更進一步瞭解色球蒸散現象，希望能推知閃焰的能量釋放情形。本篇論文研究三個閃焰事件，分別為：2014年10月27日爆發於活躍區12192的M1.7 閃焰、2014年11月9日爆發於活躍區12205的M2.3閃焰、2014年10月27日爆發於活躍區12192的X2.0閃焰，分析各事件的Mg II三種發射譜線(即Mg 2791.6 Å、 Mg II k、Mg II h)的特徵，尤其因為其中的2791.6 Å譜線對於閃焰發生的時間點非常敏感，其光強增加的時間往往能對應於硬X射線的增強，又因為該譜線的譜形比起Mg II k與Mg II h單純，因此特別針對2791.6 Å再進一步估算該譜線之各項物理參數(如溫度、線寬、都卜勒速度等)。我們的結果發現，在閃焰初期的主要能量釋放階段，2791.6 Å譜線有短暫、明顯的線寬變寬、紅移速度增加的現象，速度峰值約介於6至18 km/s，而溫度的時變曲線則較為多變。另外，我們也觀察到不同區域的譜線特徵會有所差異，可能代表不同的物理圖像。 摘要(英) Chromospheric evaporation is usually accompanied by the occurrence of solar flares. Generally, the flare-produced non-thermal electrons impact the chromosphere and heat the ambient plasma, resulting in the downward motion of thermal plasma and the subsequent chromospheric evaporation. Therefore, it is helpful to understand the physical meaning of chromospheric evaporation and the energy release process in solar flares by combining the IRIS Mg II data with the GOES soft X-ray and RHESSI hard X-ray light curves. Three flare events are investigated in this study, which are the M1.7 flare on 2014 October 27 at AR 12192, the M2.3 flare on 2014 November 9 at AR 12205, and the X2.0 flare on 2014 October 27 at AR 12192. We analyze the lightcurves of three Mg II lines (i.e., Mg 2791.6 Å, Mg II k, and Mg II h) in specific areas of each event. Moreover, since the 2791.6 line is sensitive to the heating of the lower chromosphere, responses correspondingly to the increase of hard X-ray emissions, and has a simpler spectral shape than that of Mg II k and h lines, we particularly estimate the spectral quantities of temperature, line width, and Doppler velocity from the 2791.6 line. We find that in the early impulsive phase, the red-shift velocity increases obviously and shortly with the peak value between 6 km/s and 18 km/s, as well as the broadening of line width. But the profile of temperature evolution is variable at each area. The spectral properties are observed to be different at different regions, which may indicate different physical pictures. 關鍵字(中) ★ IRIS
★ 太陽閃焰
★ Mg II譜線
★ 色球加熱關鍵字(英) ★ IRIS
★ Mg II論文目次 中文摘要 i
英文摘要 ii
致謝 iii
第一章 緒論 1
1.1 太陽結構 1
1.2 太陽閃焰與色球蒸散 3
1.3 文獻回顧與研究動機 5
第二章 分析方法 7
2.1 IRIS 7
2.1.1概述 7
2.1.2觀測模式 10
2.2 Mg II線 14
2.3 譜線參數 18
2.3.1線寬(line width) 18
2.3.2 都卜勒效應(Doppler effect) 19
2.3.3 溫度 20
第三章 事件分析結果 24
3.1事件一：2014年10月27日M1.7閃焰 24
3.1.1事件概述 24
3.1.2區域選擇 25
3.1.3光變曲線(Lightcurve) 28
3.1.4 Mg 2791.6 Å之譜線物理量 29
3.2 事件二：2014年11月9日M2.3閃焰 32
3.2.1事件概述 32
3.2.2區域選擇 33
3.2.3光變曲線 37
3.2.4 Mg 2791.6 Å之譜線物理量 39
3.3 事件三：2014年10月27日X2.0閃焰 43
3.3.1事件概述 43
3.3.2區域選擇 46
3.3.3光變曲線 50
3.3.4 Mg 2791.6 Å之譜線物理量 52
第四章 討論 58
4.1 Mg 2791.6 Å溫度計算 58
4.2 Mg 2791.6 Å與閃焰關係 63
4.3 Mg 2791.6 Å與硬X射線光變曲線關係 65
4.4 Mg II 三譜線 67
第五章 結語 71
參考資料 72參考文獻 • B. De Pontieu, A.M. Title, J.R. Lemen, G.D. Kushner, D.J. Akin, B. Allard T. Berger, P. Boerner, M. Cheung, C. Chou, J.F. Drake, D.W. Duncan S. Freeland, G.F. Heyman, C. Hoffman, N.E. Hurlburt, R.W. Lindgren, D. Mathur, R. Rehse, D. Sabolish, R. Seguin, C.J. Schrijver, T.D. Tarbell, J.-P. Wülser, C.J. Wolfson, C. Yanari, J. Mudge, N. Nguyen-Phuc, R. Timmons, R. van Bezooijen, I.Weingrod, R. Brookner, G. Butcher, B. Dougherty, J. Eder , V. Knagenhjelm, S. Larsen, D. Mansir, L. Phan, P. Boyle, P.N. Cheimets, E.E. DeLuca, L. Golub, R. Gates, E. Hertz, S. McKillop, S. Park, T. Perry, W.A. Podgorski, K. Reeves, S. Saar, P. Testa, H. Tian, M. Weber, C. Dunn, S. Eccles, S.A. Jaeggli, C.C. Kankelborg, K. Mashburn, N. Pust, L. Springer, R. Carvalho, L. Kleint, J. Marmie, E. Mazmanian, T.M.D. Pereira, S. Sawyer, J. Strong, S.P. Worden, M. Carlsson, V.H. Hansteen, J. Leenaarts, M. Wiesmann,
J. Aloise, K.-C. Chu, R.I. Bush, P.H. Scherrer, P. Brekke, J. Martinez- Sykora, 2014, The Interface Region Imaging Spectrograph (IRIS), Solar Phys, 289,2733
• H. Tian & N.-H. Chen, 2018, Multi-episode chromospheric evaporation observed in a solar flare, The Astrophysical Journal, 34, 11
• Hui Tian, Peter R. Young, Katharine K. Reeves, Bin Chen, Wei Liu, and Sean McKillop, 2015, Temporal evolution of chromospheric evaporation: case studies of the M1.1 flare on 2014 September 6 and X1.6 flare on 2014 September 10, 2015, The Astrophysical Journal, 811, 139
• Kyoung-Sun Lee, Shinsuke Imada, Kyoko Watanabe, Yumi Bamba, and David H. Brooks, 2017, IRIS, Hinode, SDO, and RHESSI Observations of a White Light Flare Produced Directly by Non-thermal Electrons, The Astrophysical Journal, 836,150
• Marina Battaglia , Lucia Kleint , Säm Krucker, and David Graham, 2015, how important are electron beams in driving chromospheric evaporation
in the 2014 March 29 flare? , The American Astronomical Society, 813,113
• Peter R. Young, Hui Tian, and Sarah Jaeggli, 2015, The 2014 March 29 X-flare: subarcsecond resolution observations of Fe XXI λ1354.1, The Astrophysical Journal, 799,218
• Q. M. Zhang , D. Li1, Z. J. Ning, Y. N. Su, H. S. Ji , and Y. Guo, 2016, Explosive chromospheric evaporation in a circular-ribbon flare, The Astrophysical Journal, 827,27
• Tiago M. D. Pereira, Mats Carlsson, Bart De Pontieu1, and Viggo Hansteen, 2015, The formation of iris diagnostics. IV. the Mg II triplet lines as a new diagnostic for lower chromospheric heating, The Astrophysical Journal, 806, 14指導教授 楊雅惠(Ya-Hui Yang) 審核日期 2018-10-1 推文 plurk
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