Abstract—

The article shows the dominant role of the global migratory flow (GMF) \({{v}_{{gmf}}} = \left\{ {v_{{gmf}}^{R},v_{{gmf}}^{\theta },v_{{gmf}}^{\varphi }} \right\}\) in the generation of the variable magnetic field of the Sun (\(v_{{gmf}}^{R}\), \(v_{{gmf}}^{\theta }\), and \(v_{{gmf}}^{\varphi }\) are the radial, meridional, and latitudinal GMF velocity components, which correspond to the velocities of the radial flow variation, spatial and temporal variation of the meridional flow, and torsional oscillations). A magnetic vector \(H^{*} = \left\{ {{{H}_{\theta }},{{H}_{\varphi }}} \right\}\), which is called a model bipolar group of spots (\({{H}_{\theta }}\) and \({{H}_{\varphi }}\) are the meridional and azimuthal components of the variable magnetic field of the Sun), is introduced. As a result of the performed numerical calculations and on the basis of the kinematic dynamo model, a scheme of the latitude–time distribution of relative amplitudes of magnetic components \({{H}_{\theta }}\) and \({{H}_{\varphi }}\) on the surface of the Sun during the 22-year magnetic cycle are constructed. It is found that the relative amplitudes of the meridional and azimuthal variable fields depend on heliolatitude. They have maximum values in the near-equatorial belt and decrease to minimum values in near-polar belts. In the near-equatorial belt, the magnetic sign of the head spot of the model bipolar group of spots coincides with the sign of the radial field in the near-polar belt. This corresponds to the ratio of the observed signs of the bipolar groups of spots and the near-polar field in the Hale magnetic cycle. At the same time, the signs of bipolar groups of spots at high heliolatitudes are in conflict with the Hale–Nicholson law. Obviously, the violation of the polarities of the vector \(H{\kern 1pt}^{*}\) can be explained by taking into account the results of simulating the dependence of the constant toroidal magnetic field on the polar angle that we obtained in previous studies. At the same time, the deviation from the Hale–Nicholson law can apparently be related to the polarity of the first high-latitude bipolar groups of spots of the new cycle observed at the end of old cycles.

中文翻译：

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全球迁移流产生太阳可变磁场

摘要-

本文显示了全球迁移流（GMF）的主导作用\（{{v} _ {{gmf}}} = \ left \ {{v _ {{gmf}} ^ {R}，v _ {{gmf}} ^ {\ theta}，v _ {{gmf}} ^ {\ varphi}} \ right \} \）在太阳的可变磁场（\（v _ {{gmf}} ^ {R} \）的生成中，\（v _ {{gmf}} ^ {\ theta} \）和\（v _ {{gmf}} ^ {\ varphi} \）是径向，子午和纬度GMF速度分量，它们对应于速度径向流变化，子午流的时空变化以及扭转振动）。磁矢量\（H ^ {*} = \ left \ {{{{H} _ {\ theta}}，{{H} _ {\ varphi}}} \ right \} \），称为模型双极点组（\（{{H} _ {\ theta}} \）介绍了\和{（{{H} _ {\ varphi}} \）是太阳可变磁场的子午和方位分量）。作为进行了数值计算的结果，并基于运动学发电机模型，提出了磁性成分\（{{H} _ {\ theta}} \）和\（{ {H} _ {\ varphi}} \）构造了在22年的磁循环中太阳表面的光。发现子午和方位角可变场的相对振幅取决于日高。它们在近赤道带中具有最大值，而在近极带中具有最小值。在近赤道带中，模型双极点组的头部磁头的磁符号与近极带中径向场的符号重合。这对应于黑尔磁循环中的双极点组的观察到的符号与近极场的比率。同时，在高直度下双极点的迹象与黑尔-尼科尔森定律相冲突。显然，违反了向量\（H {\ kern 1pt} ^ {*} \）的极性可以通过考虑我们在先前研究中获得的模拟恒定环形磁场对极角的依赖性来解释。同时，与Hale-Nicholson定律的偏差显然可以与旧周期结束时观察到的新周期的第一个高纬度双极群的极性有关。