夜間溫度極大 (Midnight Temperature Maximum, MTM)主要是一種發生在夜間低緯度的高層大氣效應，會在接近午夜時造成溫度明顯變化，進而影響到中低電離層的電漿活動，而溫度變化的差距相當的廣泛，依據過去觀測的結果，溫差甚至可高達200度F左右[Colerico and Mendillo, 2002; Meriwether et al., 2008]。在夜間溫度極大異常效應發生後往往都會伴隨著壓力的增加，因而從靠近赤道的壓力區因壓力梯度的關係產生向兩極區方向的子午風(meridional neutral wind);同時，從過去的地面觀測發現，午夜的630.0 nm波段暉光也會隨著溫度極大異常現象而出現明顯的增強，一般稱此向極區方向移動的暉光亮區為午夜亮區波動現象(Midnight Brightness Waves, MBW) [Colerico et al., 1996]，這兩者之間無論是產生的位置和移動特徵，都有著相當高的一致性。雖然過去的觀測已證明這兩者之間的高度相關性，但卻對這兩者之間的連結論述交代不清，尤其是MTM的產生原因和暉光亮區的生成機制都還是未解之謎，所以，我們相信必定有一些物理機制尚待提出或是模擬方法需要修正，而這就是進行本研究論文的動機所在。
以往的夜間暉光觀測都是以地面觀測為主要工具，但這會受限於氣候和環境的變化，所以本研究是利用衛星觀測來進行。衛星觀測不受天氣與區域的限制，可以進行全球的夜間暉光分布調查，所以它的長期觀測的統計結果有非常高的準確度和參考價值。在這個研究中，我們選擇台灣的福衛二號所搭載的ISUAL科學儀器來當作我們的工具，進行為期兩年的全球觀測任務。為了能對夜間暉光亮區的物理機制得到決定性的證據，我們除了對全球暉光的分布與趨勢行為做定性分析外，還做了定量分析統計，並依據不同特性條件將所有事件分為四種類型，依據每種類型的發生率所呈現的半年度週期與年度週期性的結果，來進行背景物理機制的討論。
為了進一部探討夜間溫度極大異常現象背後可能的形成機制與它所影響的程度，我們利用SAMI-2模型，探討溫度變化對暉光強度的影響程度；此外，我們調整模型中的中性風場，模擬帶電粒子在正常風場與關閉風場影響下的差別。而在比對溫度與風場兩者之間的影響權重關係下，我們進行了詳細的驗證和說明，並成功得到兩變數的影響數值方程式，可利用於未來模型的建構上。
關於最關鍵的問題，夜間溫度極大異常現象的產生機制，我們在這一系列的研究中也提出模擬上的基礎修正，以融入過去研究中所忽略的物理作用。為了瞭解中性粒子在kinetic approach和碰撞條件下能否造成溫度上的變化，我們在這個研究中將中性粒子的速度分布做Maxwell-Boltzmann的近似。而從我們建構的模型中，初步模擬的結果來看是相當正面的，在中性風的驅動之下，已可以成功產生中性粒子在溫度上的改變。在未來的工作中，我們將持續修正模型設定，盡力達到所有背景環境和作用過程都趨近真實的情境，最終目標是希望能建立一個全動力學的電離層模型。

Midnight Temperature Maximum (MTM) is mainly an upper atmospheric effect that occurs at low latitudes, which causes a significant temperature anomaly near midnight. Then it induces plasma variations in the low- and middle-latitude ionosphere. The temperature difference is quite large and can be as high as 200 K according to past observations [Colerico and Mendillo, 2002; Meriwether et al., 2008]. After the MTM effect occurs, it is often accompanied by an increase in pressure near the equator, with the associated pressure gradient causing meridional neutral wind from the equator to the polar region. At the same time, from past ground observations, it was found that the 630.0 nm nightglow near midnight also increased significantly with the MTM effect. Generally, this nightglow brightness moving toward the polar regions is called Midnight Brightness Waves (MBW) [Colerico et al., 1996]. Regardless of the generated position and movement characteristics, there is a fairly high degree of consistency. Although the past observations have proven a high correlation between the two phenomena, the physical connection between them is unclear. In particular, the causes of the MTM and the mechanism of brightness are still unsolved. Therefore, we believe that there must be some physical mechanism to be proposed or the simulation method needs to be revised, and this is the motivation for carrying out this research.
In the past, observations of nightglow were mainly made from the ground, but this kind of studies is limited by changes in climate and environment. In this study, we adopted satellite observations which are not limited by weather and geographic area, and thus we could perform surveys of the global nightglow distribution. We selected the ISUAL scientific instrument onboard Taiwan's FORMOSAT-2 as our tool for a two-year global observation study. With the goal of understanding the physical mechanism of the nightglow brightness, we performed qualitative analysis of the global nightglow distribution and trend behavior. Furthermore, we conducted quantitative statistical analysis. We divided all available events into four categories based on the different characteristics, and discussed the mechanism based on the semi-annual and annual periodic results of each types.
In order to further explore the possible formation mechanism of MTM and its influence, we simulated the relevant ionospheric conditions based on the SAMI-2 model. By changing the temperature in the simulations, we could understand its influence on nightglow emission. Besides, the neutral wind condition is also changed in the simulations. Considering the influence of temperature and the neutral wind, we carried out detailed verification and explanations, and successfully obtained numerical formula involving the two parameters, which can be used in the construction of future models.
Regarding the most critical issue, the mechanism for the occurrence of MTM, we have also proposed basic modifications to simulations in this series of studies, which incorporate physical effects that have been ignored in previous studies. In order to understand whether neutral particles can cause temperature changes under kinetic approach and collisional conditions, we make the Maxwell-Boltzmann approximation of the velocity distribution of particles in this study. From the model we constructed, the results of the preliminary simulations are quite positive. Driven by the neutral wind, the temperature variations of the neutral particles can be successfully produced. In the future work, we will continue to revise the model settings and try to achieve a situation where all background environments and interaction processes are close to reality. The ultimate goal is to build a fully kinetic ionospheric model.

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