Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles
Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles
复制标题
太阳周期大尺度磁场纬度带状结构的演化
DOI：
10.1007/bf00146210
复制
发表时间：
1989
期刊：
影响因子：
2.8
通讯作者：
K. Sivaraman
中科院分区：
文献类型：
--
作者：
V. Makarov;K. Sivaraman
根据1905-1982年的Hα图，分析了大尺度太阳磁场的纬向分量的性质。日珥向极地迁移被用来确定1870-1905年极磁场反转的时间。结果表明，通过计算大尺度磁场某一边界的日珥样本的平均纬度，可以探测到各半球大尺度磁场主极性的极区、中纬度区和赤道区。研究了单极性和三极性磁场反转的情况。结果表明，在大尺度磁场的一个边界处，日珥样品不存在规律性的赤道漂移。它们表现出向极地迁移的变化速度，根据周期的阶段可达30米每秒1。低纬度和高纬度地区的迁移方向相同。发现了两个不同的向极地迁移时间间隔。一个从周期开始持续到极磁场反转时间，另一个从反转时间持续到活动最小时间。第一阶段日珥向极迁移的速度在5 ~ 30 m s-1之间，第二阶段没有规律的纬度漂移。
Properties of a latitude zonal component of the large-scale solar magnetic field are analyzed on the basis of Hα charts for 1905–1982. Poleward migration of prominences is used to determine the time of reversal of the polar magnetic field for 1870–1905. It is shown that in each hemisphere the polar, middle latitude and equatorial zones of the predominant polarity of large-scale magnetic field can be detected by calculating the average latitude of prominence samples referred to one boundary of the large-scale magnetic field. The cases of a single and three-fold polar magnetic field reversal are investigated. It is shown that prominence samples referred to one boundary of the large-scale magnetic field do not have any regular equatorward drift. They manifest a poleward migration with a variable velocity up to 30 m s-1 depending on the phase of the cycle. The direction of migration is the same for both low-latitude and high-latitude zones. Two different time intervals of poleward migration are found. One lasts from the beginning of the cycle to the time of polar magnetic field reversal and the other lasts from the time of reversal to the time of minimum activity. The velocity of poleward migration of prominences during the first period is from 5 m s-1 to 30 m s-1 and the second period is devoid of regular latitude drift.