模擬極端太陽風暴事件發生期間，月球鈉外氣層分佈情形

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姓名

陳政憲(Zheng-Xian Chen) 查詢紙本館藏

畢業系所

太空科學研究所

論文名稱

模擬極端太陽風暴事件發生期間，月球鈉外氣層分佈情形
(Simulating the distribution of the lunar sodium exosphere during the extreme solar storm event)

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摘要(中)

與月球外氣層相關的研究已有許多的成果，但是針對太陽風暴事件發生期間月球外氣層隨時間變化的研究則相對較少，因此我們利用環繞月球的ARTEMIS衛星上的固態望遠鏡(Solid State Telescope, SST)，獲得太陽風暴發生期間近月球太空環境的能量通量，計算出太陽風暴發生期間鈉原子的隨時間變化的產量。接著，我們使用蒙地卡羅方法(Monte-Carlo method)模擬鈉原子在近月球太空環境中傳輸與消散的彈跳軌道。同時，也利用能量平衡方程式計算月球的全球表面溫度，以利於模擬鈉原子在撞擊月球表面時的反應結果。利用鈉原子軌跡的模擬結果我們可以分別得到月球鈉外氣層在穩定狀態下與產生鈉原子後不同時段的密度分布，最後，我們再結合上述結果與計算所得的太陽風暴發生期間鈉原子產量，我們便可以得到太陽風暴事件發生時月球鈉外氣層柱密度分佈隨時間變化的模擬結果，相信利用該結果可以對未來月球衛星任務有所幫助。

摘要(英)

There have been many studies related to the lunar exosphere, but there have been relatively few studies on the changes with time of the lunar exosphere during the solar storm. Therefore, we use the Solid State Telescope (SST) on the ARTEMIS satellite around the moon to obtain the energy flux of the near-moon space environment during the solar storm, and calculate the time-dependent production of sodium atoms during the solar storm. Next, we use the Monte-Carlo method to simulate the bounce trajectory of sodium atoms transporting and dissipating in the near-moon space environment. At the same time, the energy balance equation is also used to calculate the global surface temperature of the moon to facilitate the simulation of the reaction results when sodium atoms hit the surface of the moon. Using the simulation results of the sodium atom trajectory, we can obtain the density distribution of the lunar sodium exosphere at the steady state and time dependent, respectively. Finally, we combine the above results with the calculated sodium atom yield during the solar storm. We can obtain the simulation results of the distribution of the density of the lunar sodium exosphere over time during the solar storm event. It is believed that this result can be helpful for future lunar satellite missions.

關鍵字(中)

★ 月球
★ 外氣層
★ ARTEMIS衛星

關鍵字(英)

★ Moon
★ Exosphere
★ ARTEMIS satellite

論文目次

摘要………………………………………………………………………………　　ⅰ
Abstract…………………………………………………………………………　　ⅱ
致謝………………………………………………………………………………　　ⅲ
目錄………………………………………………………………………………　　ⅴ
圖目錄……………………………………………………………………………　　ⅶ
表目錄……………………………………………………………………………　　ⅹⅲ

第1章緒論……………………………………………………………………………　　1
1.1 月球外氣層中性原子來源與產生機制………………………………………　　2
1.1.1 流星體撞擊汽化……………………………………………………　　3
1.1.2 光子激發解吸………………………………………………………　　4
1.1.3 離子濺射……………………………………………………………　　4
1.2 觀測……………………………………………………………………………　　5
1.2.1 地面觀測……………………………………………………………　　5
1.2.2 實地觀測……………………………………………………………　　8
1.3 ARTEMIS衛星…………………………………………………………………　　13
1.3.1 任務………………………………………………………………...　　13
1.3.2 儀器………………………………………………………………...　　17
1.3.3 月球環境…………………………………………………………...　　20
1.3.3.1 進入地球磁層裡……………………………………………..　　22
1.3.3.2 位於平靜太陽風……………………………………………..　　23
1.3.3.3 當太陽風暴發生……………………………………………..　　23
1.3.4 太陽風暴事件數據………………………………………………..　　23
第2章月球外氣層模型……………………………………………………………...　　31
2.1 月球表面熱模型……………………………………………………………..　　32
2.1.1 熱傳導方程式……………………………………………………...　　33
2.2 月球外氣層鈉原子軌跡模型………………………………………………..　　36
2.2.1 粒子移動…………………………………………………………...　　39
2.2.1.1 太陽輻射壓力………………………………………………...　　39
2.2.2 表面交互作用……………………………………………………...　　39
2.2.2.1 粒子反彈……………………………………………………...　　39
2.2.2.2 再發射………………………………………………………...　　40
2.2.2.3 冷阱…………………………………………………………...　　40
2.2.3 結束模型…………………………………………………………...　　40
2.2.3.1 粒子逃逸……………………………………………………...　　41
2.2.3.2 光電離………………………………………………………...　　41
2.2.3.3 冷阱…………………………………………………………...　　41
2.2.4 高速組……………………………………………………………...　　47
2.2.5 低速組……………………………………………………………...　　48
第3章結果…………………………………………………………………………...　　49
3.1 穩定狀態……………………………………………………………………..　　50
3.2 時間變化……………………………………………………………………..　　53
3.3 極端太陽風暴………………………………………………………………..　　57
第4章總結與討論…………………………………………………………………...　　60
第5章參考書目……………………………………………………………………...　　65
附錄A……………………………………………………………………………………　　68

參考文獻

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網站
https://umbra.nascom.nasa.gov/SEP/
http://artemis.ssl.berkeley.edu/index.shtml
https://www.nasa.gov/mission_pages/ladee/main/index.html
https://www.nasa.gov/themis-and-artemis

指導教授

葉永烜(Wing-Huen Ip)

審核日期

2019-8-21

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