目前观测得到的日冕物质抛射(coronal mass ejection,CME)只是其在天空平面的投影,其观测参量与真实参量之间存在一定的差异。而CME的速度是对其地磁效应有决定性影响的参量,因此对CME测量速度作投影效应改正是一个重要的研究课题。综述了近年来对CME测量速度进行投影效应改正的方法,并指出了这些投影效应改正方法中存在的一些问题和进一步的研究方向。
利用Carte Synoptique solar filament archive的暗条观测资料研究了高纬度太阳活动的纬度漂移.定量分析了高纬度活动的两种漂移:已知的太阳活动从中纬度(40°)向太阳两极的纬度漂移,以及新发现的从太阳两极向太阳中纬度的纬度漂移.在一个太阳活动周内从中纬度向太阳两极的纬度漂移的时间(约4.4a)比从太阳两极向太阳中纬度的纬度漂移的时间(约6.6a)要短约2.2a,这两种漂移的转换发生在太阳活动的极大期.将来,太阳活动发电机理论要考虑这种从太阳两极向太阳中纬度的纬度漂移.太阳活动延伸周是从太阳两极向太阳赤道的连续纬度漂移活动周的一部分.
Utilized here is the Carte Synoptique solar filament archive, namely the catalogue of solar filaments from March 1919 to December 1989, corresponding to solar rotation numbers 876 to 1823 to study latitudinal migration of solar activity at high latitudes. Except the well-known poleward migration of solar activity from middle latitudes to the poles, an equatorward migration is found from the solar poles toward middle latitudes (about 40°) within a normal cycle, which is neglected before, and the time in-terval for the former migration (4.4 years) is about 2.2 years shorter than that for the latter (6.6 years), indicating that the change from one migration to the other takes place around the maximum time of a normal cycle. In the future, a dynamo model should represent the migration from the poles toward middle latitudes of the Sun, besides the migration in "butterfly diagrams" and the "rush to the poles". The traditional extended activity cycle is actually a part of the period of the successive migration from the poles toward the solar equator.
