We study the role of drift effect in the temporal changes of the anisotropy of galactic cosmic rays (GCRs) and the influence of the sector structure of the heliospheric magnetic field on it. We analyze the GCRs anisotropy in the Solar Cycle 24 and solar minimum 23_24 with negative polarity for the period of 2007-2009 and near minimum 24_25 with positive polarity in 2017-2018 using data of global network of Neutron Monitors. We use the harmonic analyses method to calculate the radial and tangential components of the anisotropy of GCRs for different sectors (plus corresponds to the positive and minus to the negative directions) of the heliospheric magnetic field. We compare the analysis of GCRs anisotropy using different evaluations of the mean GCRs rigidity related to Neutron Monitor observations. Then the radial and tangential components are used for characterizing the GCRs modulation in the heliosphere. We show that in the solar minimum 23_24 in 2007-2009 when negative, the drift effect is not visibly evident in the changes of the radial component, i.e. the drift effect is found to produce 4 % change in the radial component of the GCRs anisotropy for 2007-2009. Hence the diffusion dominated model of GCRs transport is more acceptable in 2007-2009. In turn, near the solar minimum 24_25 in 2017-2018 when positive, the drift effect is evidently visible and produce 40% change in the radial component of the GCRs anisotropy for 2017-2018. So in the period of 2017-2018 diffusion model with noticeably manifested drift is acceptable. The results of this work are in good agreement with the drift theory of GCRs modulation, according to which during negative (positive) polarity cycles, a drift stream of GCRs is directed toward (away from) the Sun, thus giving rise to a 22-year cycle variation of the radial GCRs anisotropy.
Quantifying the Anisotropy and Solar Cycle Dependence of "$1/f$" Solar Wind Fluctuations Observed by Ace
演变中的太阳风的功率谱显示了在较高频率的湍流波动的惯性范围和较低频率的“$1/f$“状区域之间的谱断裂的证据。在$\sim 1$ AU的黄道面上，这种破裂大约发生在几个小时的时间尺度上，并在速度和磁场分量的功率谱中观察到。“$1/f$“的能量范围比惯性范围更直接的日冕起源，并携带复杂的太阳日冕磁场结构的签名，并在太阳光球的脚点搅拌。为了量化的标度特性，我们使用通用的统计方法，如广义结构函数和PDF，专注于太阳周期的依赖性和各向异性的背景磁场。我们提出了结构函数分析的磁场和速度场的波动，使用一种新的技术来分解的波动方向平行和垂直于平均本地背景磁场。虽然磁场接近“$1/f$“，我们表明，速度场是“$1/f^α$“与$α\neq1$。对于速度，$α$的值在平行和垂直波动之间变化，并随太阳活动周期变化。$α$也随太阳风速度而变化。我们已经研究了快速、安静的太阳风中的PDF，有趣的是，虽然平行和垂直是不同的，但${\boldmath$ B $}$场和速度都显示出相同的垂直波动PDF，这接近于伽马或逆Gumbel。这些结果指出了日冕中不同的物理过程，以及它们映射到太阳风中的过程。得到的标度指数约束这些过程的模型。
Long term variation of the solar diurnal anisotropy of galactic cosmic rays observed with the Nagoya multi-directional muon detector
我们分析了银河宇宙线（GCR）强度的三维各向异性独立观察在日本名古屋的μ子探测器和中子监测器在四个太阳活动周期。我们清楚地看到，由于平行于平均磁场的各向异性分量减少，在A>0的历元中，自由空间的周日各向异性的相位在太阳活动最小值附近向更早的几个小时移动。平均平行分量与刚度无关谱一致，而垂直分量随GCR刚度增加而增加。我们认为，这种更硬的垂直分量的光谱是由于漂移流的贡献。结果表明，在A>0时，双向纬向密度梯度为正，而在A<0时，双向纬向密度梯度为负，这与漂移模型的预测相一致。另一方面，径向密度梯度的变化周期约为11年，在太阳活动的极大（极小）期出现极大（极小）值，但在A>0和A<0的历元中，平均径向梯度没有显著差异。平均平行平均自由程在A0处较大<0 than in A>.然而，我们也发现，平行平均自由程（径向梯度）似乎持续增加（减少）在过去三个周期的太阳活动减弱。我们认为，这些参数之间的简单差异在A>0和A<0的时代是严重的偏见，这些长期趋势。
A Solar Dynamo Model Driven by Mean-Field Alpha and Babcock-Leighton Sources: Fluctuations, Grand-Minima-Maxima and Hemispheric Asymmetry in Sunspot Cycles
WawHelioGlow: a model of the heliospheric backscatter glow. II. The helioglow buildup and the potential significance of the anisotropy in the solar EUV output
Recovery of the Solar Cycle from Maunder-like Grand Minima Episodes: A Quantification of the Necessary Polar Flux Threshold through Solar Dynamo Simulations
Recurrence of galactic cosmic rays intensity and anisotropy in solar minima 23/24 and 24/25 by ACE/CRIS, STEREO, SOHO/EPHIN and neutron monitors. Fourier and wavelet analysis. Dedicated to the Memory of Michael Alania
目标。利用中子监测仪（NM）、ACE/CRIS、STEREO和SOHO/EPHIN观测资料，研究了23/24和24/25日太阳磁周期极性相反的极小期银河系宇宙射线（GCR）的27天变化。现在有机会重新分析2007-2009年负A0的周期性GCR变化幅度的极性依赖性< 0 solar magnetic polarity and to compare it with the clear periodic variations related to solar rotation in 2017-2019 for positive A >。方法.我们用傅里叶分析方法研究了GCR通量的周期性。由于GCR复发是太阳自转的结果，我们不仅分析GCR通量，但也太阳和日光层参数检查27天GCR变化和日光层之间的关系，以及太阳风参数。结果我们发现，NMs数据的GCR强度和各向异性的27天变化的振幅的极性依赖性在最后两个太阳极小期：23/24（2007-2009）和24/25（2017-2019）中保持不变，在正A > 0的太阳磁极性中振幅更大。ACE/CRIS、SOHO/EPHIN和STEREO测量不受正A > 0极性中更大振幅的原理的支配。对于低能（< 1GeV）宇宙射线，太阳自转引起的GCR重现对增强扩散效应更为敏感，导致正负极的27天振幅处于同一水平。而NMs记录的高能（>…
