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Height Stratification and Polar Reversal of the Sun's Magnetic Fields in Cycles 21-23

机译：周期21-23中太阳磁场的高度分层和极性反转

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摘要

Using calculations of the magnetic field in the solar atmosphere in the potential approximation, it is shown that, (1) as distance R from the Sun's center grows, the area of the positive magnetic field (S_(+field)) in 10-deg latitude zones tends to 100% (0%) in the neighborhood of the solar minimum. At the distance R = 2.5R_⊙ (R_⊙ is the solar radius), these values of the positive field are observed during ≈(12-55) Carrington rotations (CRs) for solar minima between neighboring cycles; (2) polar magnetic field reversals can occur repeatedly. Note that a polar reversal at large heights ends by 6-16 Carrington rotations earlier than on the Sun's surface. On the Sun's surface, a field polar reversal begins earlier at lower latitudes than at high ones; (3) for each longitude at different Rs and separately for each solar hemisphere the radial component of the field was averaged on synoptic maps in the 0°-40° latitude range. It is established that the T_R rotation periods of the boundaries between the sectors (areas of longitudes with the same sign of the averaged field) can be shorter than, longer than, and equal to Carrington solar rotation period T_(CR). It turned out that boundaries with T_R < T_(CR) are observed at all heights, while boundaries with T_R > T_(CR) are observed at relatively small heights.
机译：使用电势近似法计算太阳大气中的磁场，结果表明：（1）随着距太阳中心的距离R的增大，正磁场的面积（S _（+ field））为10度最低纬度附近的纬度区域趋向于100％（0％）。在距离R =2.5R_⊙（R_⊙是太阳半径）时，在≈（12-55）卡林顿旋转（CRs）期间，在相邻周期之间的太阳极小值时观察到这些正场值。 （2）极性磁场反转可以反复发生。请注意，大高度的极地逆转比太阳表面早6-16卡林顿旋转结束。在太阳的表面上，磁场的极地逆转始于低纬度，而不是高纬度。 （3）对于在不同Rs的每个经度，以及对于每个太阳半球，分别在0°-40°纬度范围内的天气图上将视场的径向分量平均。已经确定，扇区之间的边界的T_R旋转周期（具有平均场的相同符号的经度区域）可以小于，大于或等于卡林顿太阳旋转周期T_（CR）。事实证明，在所有高度都观察到T_R T_（CR）的边界。

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