日珥在太陽表面是一個特殊的現象。直到目前為止，日珥的形成原因一直都還沒有定論。在本論文研究中，我們由全球資訊網（WWW）取得了1998年與1999年的地面觀測之Hα影像資料以及衛星觀測之MDI（Michelson Doppler Imager）、EIT（Extreme Ultraviolet Imaging Telescope）、SXT（Soft X-ray Telescope）等影像資料。我們根據Hα影像資料決定日珥在太陽全球的分佈情形與形貌特徵。並根據日珥的緯度分佈與形貌特徵加以分類。我們再配合MDI、EIT、SXT等影像資料，分析各類型日珥的上方日冕結構與背景磁場強度。我們由資料分析的結果推論：除了Radiative cooling instability可形成日珥外，Kelvin-Helmholtz instability、magnetic buoyancy instability和Rayleigh-Taylor instability等三種機制在日珥的形成過程中，應該也扮演著重要的角色。 Prominences are distinct phenomena on solar disk. However, the physical processes that can lead to formation of solar prominences are not fully understood yet. In this study, we obtain observational data from websites. These data include Hα image data from ground-based observatories as well as MDI (Michelson Doppler Imager), EIT (Extreme Ultraviolet Imaging Telescope) and SXT (Soft X-ray Telescope) image data from SoHO and Yohkoh satellites’ observations. We analyze Hα data obtained during 1998 and 1999 to determine the distribution and shape of prominences on solar disk. We classify the observed prominences into several types according to their latitudinal distribution and their shape. For each type of prominences, we analyze the coronal structure above them and the line-of-sight magnetic field intensity around them based on MDI, EIT and SXT images. Based on our analysis, we infer that besides radiative cooling instability, the Kelvin-Helmholtz instability, magnetic buoyancy instability and Rayleigh-Taylor instability should also play important roles on the formation of solar prominences.
