论文标题
太阳差异旋转和黑子活性的长期变化，II：围绕太阳能循环的最大值和最小值12-24的差异旋转
Long-Term Variations in Solar Differential Rotation and Sunspot Activity, II: Differential Rotation Around the Maxima and Minima of Solar Cycles 12-24
论文作者
论文摘要
我们分析了1874 - 1976年期间Greenwich Photoheliogrphic结果（GPR）报告的黑子组每日数据，并在1977 - 2017年期间分析了1874- 1976年期间的光旋光数据（DPD）。我们通过在3年移动时间间隔（3年MTIS）中拟合数据，在1874 - 2017年期间，将数据连续移动一年，以确定太阳差旋转旋转的赤道旋转速率[a]和纬度梯度[B]成分。 A和B的值大约在太阳周期的最大值和最小值12-24的年代中，是从A和B的3年MTIS系列中获得的，并研究了这些系数中的长期循环到周期调制。在这里，我们使用了最近从修订版的2版Internation International Sunspot-Number系列中确定的太阳能周期的最大值和最小值的时期。我们发现，在太阳循环的最大值周围的A最大值中出现了相当显着的世俗减少趋势。在太阳周期的最小值周围的A和B中都没有世俗的趋势。在统计学上，太阳周期最大周围的B的世俗趋势在统计学上是微不足道的。消除了相应的线性趋势后，我们将余弦函数拟合到A的值以及B的值。余弦表明，在太阳能周期的最大值和最小值周围的A（b）中，存在〜54年（〜94年）和〜82年（〜79年）。 A（B）周围的A（B）余弦曲线的幅度约为Maxima周围A（B）的41％（65％）。此外，A和B的余弦曲线表明，A和B之间的长期变化之间存在很大（最高180度）的相位差异，也表明了B的长期变化，最大值和太阳周期的最小值。
We analyzed the sunspot-group daily data that were reported by Greenwich Photoheliogrphic Results (GPR) during the period 1874-1976 and Debrecen Photoheliographic Data (DPD) during the period 1977-2017. We determined the equatorial rotation rate [A] and the latitude gradient [B] components of the solar differential rotation by fitting the data in each of the 3-year moving time intervals (3-year MTIs) successively shifted by one year during the period 1874-2017 to the standard law of differential rotation. The values of A and B around the years of maxima and minima of Solar Cycles 12-24 are obtained from the 3-year MTIs series of A and B and studied the long-term cycle-to-cycle modulations in these coefficients. Here we have used the epochs of the maxima and minima of Solar Cycles 12-24 that were recently determined from the revised Version-2 international sunspot-number series. We find that there exits a considerably significant secular decreasing-trend in A around the maxima of solar cycles. There exist no secular trends in both A and B around the minima of solar cycles. The secular trend in B around the maxima of solar cycles is also found to be statistically insignificant. We fitted a cosine function to the values of A, and also to those of B, after removing the corresponding linear trends. The cosine-fits suggest that there exist ~54-year (~94-year) and ~82-year (~79-year) periodicities in A (B) around the maxima and minima of solar cycles, respectively. The amplitude of the cosine-profile of A (B) around the minima of solar cycles is about 41% (65%) larger than that of A (B) around the maxima. In addition, the cosine profiles of A and B suggest a large (up to 180 degree) phase difference between the long-term variations of A, and also between those of B, around maxima and minima of solar cycles.
