|Variability of Extended Bipolar Regions|
|Song, W. B.; Feng, X. S.; Shen, F.; Zhang, Y. Z.; 北京8701信箱
|Source Publication||Solar Physics
|Abstract||Using NSO/Kitt Peak synoptic charts from 1975 to 2003, we group the main solar magnetic fields into two categories: one for active regions (ARs) and the other for extended bipolar regions (EBRs). Comparing them, we find that there exist three typical characteristics in the variability of EBRs: First, there exists a correlation between ARs and EBRs. The phase of EBR flux has a delay nearly two CRs. Second, we find that the EBR flux has two prominent periods at 1.79 years and 3.21 years. The 1.79-year period seems to only belong to large-scale magnetic features. Lastly, the North -aEuro parts per thousand South asymmetry of EBR flux is not very significant on a time scale of one solar cycle. However, during solar maxima, its dominance is found to shift from one hemisphere to the other.|
Song, W. B.,Feng, X. S.,Shen, F.,et al. Variability of Extended Bipolar Regions[J]. Solar Physics,2009,257(1):83-90.
Song, W. B.,Feng, X. S.,Shen, F.,Zhang, Y. Z.,&北京8701信箱.(2009).Variability of Extended Bipolar Regions.Solar Physics,257(1),83-90.
Song, W. B.,et al."Variability of Extended Bipolar Regions".Solar Physics 257.1(2009):83-90.
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