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Study of the Diurnal Variation of Cosmic Rays during Different Phases of Solar Activity

机译：太阳活动不同阶段宇宙射线日变化的研究

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The pressure-corrected hourly counting rate data of ground-based super neutron monitor stations, situated in different latitudes, have been employed to study the characteristics of the long-term variation of cosmic-ray diurnal anisotropy for a long (44-year) period (1965 - 2008). Some of these super neutron monitors are situated in low latitudes with high cutoff rigidity. Annual averages of the diurnal amplitudes and phases have been obtained for each station. It is found that the amplitude of the diurnal anisotropy varies with a period of one solar activity cycle (11 years), whereas the diurnal phase varies with a period of 22 years (one solar magnetic cycle). The average diurnal amplitudes and phases have also been calculated by grouping the days on the basis of ascending and descending periods of each solar cycle (Cycles 20, 21, 22, and 23). Systematic and significant differences are observed in the characteristics of the diurnal variation between the descending periods of the odd and even solar cycles. The overall vector averages of the descending periods of the even solar cycles (20 and 22) show significantly smaller diurnal amplitudes compared to the vector averages of the descending periods of the odd solar cycles (21 and 23). In contrast, we find a large diurnal phase shift to earlier hours only during the descending periods of even solar cycles (20 and 22), as compared to almost no shift in the diurnal phase during the descending periods of odd solar cycles. Further, the overall vector average diurnal amplitudes of the ascending period of odd and even solar cycles remain invariant from one ascending period to the other, or even between the even and odd solar cycles. However, we do find a significant diurnal phase shift to earlier hours during the ascending periods of odd solar cycles (21 and 23) in comparison to the diurnal phase in the ascending periods of even solar cycles (20 and 22).
机译：已使用位于不同纬度的地面超级中子监测站的压力校正后每小时计数率数据来研究宇宙射线日向各向异性长期（44年）的长期变化特征（1965年-2008年）。这些超级中子监测仪中的一些监测仪位于低纬度，高截止刚度。每个站的日均振幅和相位的年度平均值已经获得。发现日各向异性的幅度随一个太阳活动周期（11年）的周期而变化，而日相则随22年周期（一个太阳磁周期）的变化而变化。还通过根据每个太阳周期（周期20、21、22和23）的上升和下降时间对天数进行分组来计算平均日振幅和相位。在奇数和偶数太阳周期的下降周期之间的日变化特征中观察到系统的显着差异。与奇数太阳周期（21和23）的下降周期的矢量平均值相比，偶数太阳周期（20和22）的下降周期的矢量平均值显示出明显更小的日振幅。相比之下，我们发现仅在偶数太阳周期（20和22）的下降期间，有较大的昼夜相移，而在奇数太阳周期的下降期间，昼夜相几乎没有变化。此外，奇数和偶数太阳周期的上升周期的总体矢量平均日振幅从一个上升周期到另一个上升周期，或者甚至在偶数和奇数太阳周期之间保持不变。但是，我们确实发现，与偶数太阳周期（20和22）的上升周期中的昼夜相相比，在奇数太阳周期（21和23）的上升周期中有明显的昼夜相移。

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