日冕物質拋射在行星際空間所形成的磁雲與電漿氣泡，對太空氣候有密切的影響。而日冕物質拋射的發生，源自於太陽表面的強磁場活躍區。為了瞭解日冕物質拋射事件的發生頻率，與磁場活躍區的生命週期裡的關係？所以我們選定接近太陽極小期的2005 年，使用方位角配對的方式，找出124個CME 與其相關的磁場活躍區。並檢視邁克森都卜勒磁像儀影像，追蹤壽命長於一個太陽自轉週期的磁場活躍區，得到39 個案例。最後，我們挑選出11 個至少發生兩次CME 的長週期磁場活躍區進行分析。結果發現：(1) CME 的發生次 數隨著活躍區壽命的增長而無明顯變化、(2)CME 的發生在活躍區的生命週期裡隨機出現，沒有特別集中的情況、(3)單一活躍區引發的非暈狀CME 屬於慢速CME。 Coronal mass ejection events (CMEs) characterized by the formation of magnetic clouds and plasma bubbles in the interplanetary space are closely related to the study of space weather. In order to investigate the correlation of CMEs with the corresponding active regions (ARs), we have performed a statistical study of the time evolution of a number of active regions with the production of at least one CME in 2005 when was close to the recently solar minimum (Oct 2008). We use the CMEs catalogue from LASCO (Large Angle and Spectrometric Coronagraph experiment) on the SOHO spacecraft and the Solar Region Summary(SRS) from the Space Weather Prediction Center (SWPC) of National Oceanic and Atmospheric Administration (NOAA) to find out the CME source region. The statistical study includes analysis of CME distribution over the lifetime of active regions, racing long-term active regions from the MDI (Michelson Doppler Imager). The results are: (1) The distribution of CME is relatively uniform over each active regions, (2) the amount of CME occurrence is not proportional to the AR's lifetime, (3)the CME corresponding to single active region is slow(less than 1000 Km/s).
