大氣輝光是發生在高層大氣中氣層及熱氣層的一種化學發光現象。由於此發光化學反應和高層大氣參數有正相關，所以可以藉由大氣輝光的亮度變化去反演出高層大氣的相關參數，例如氧原子的濃度、高層大氣的溫度或風場的變化等。因為此原因我們正發展一套簡易觀測大氣輝光的光度計系統，目前已經組裝完成並且成功校正完儀器，並計畫要在鹿林山進行長期觀測。在這套系統中，我們選擇557.7奈米、589奈米、630奈米，作為我們觀測大氣輝光的目標波長，原因是因為這三種大氣輝光過去有許多相關研究，以利我們進行資料的驗證。為了要取得可靠性較高的觀測資料，我們必須驗證每一個環節，從發展、儀器設計、儀器校正到資料處理都必須詳細驗證及測試。 我們已經利用標準光源及積分球完成系統在不同觀測頻道對不同輻射度光源的響應，目前也持續在進行夜間大氣輝光的觀測活動。在未來，我們將利用觀測資料與高層大氣現象進行比對並確認中氣層與熱氣層之間的化學轉換關係。在確認我們觀測資料是可靠的之後，我們將會在鹿林山天文台進行長期觀測以及監測台灣上空大氣輝光與化學變化過程。 ;Airglow is a phenomenon caused by chemical reactions in the mesosphere and thermosphere, and can also be used as a proxy to measure important parameters in upper atmosphere. Due to this reason, we have built a simple airglow photometer system and plan to deploy it for long term ground-based observations at Lulin Observatory. We have selected three airglow emission channels (557.7nm, 589nm, 630nm) as our observation target, which have been the subject of several past studies. In order to get reasonable data from our airglow observations, we need to validate all parts of our system, design, calibration, and the data processing procedure. We have used an integrating sphere to determine the response of our photometer to different levels of irradiance at different channels, and have performed three nights of airglow observations. In the future, we will use our observation results to compare with some atmospheric events and determine chemical changes in the mesosphere and thermosphere. After demonstrating that the data we use is reliable, we will provide long-term observations and monitoring of airglow emission rates and chemical processes over Taiwan.
