论文标题
太阳活动和短暂区域的旋转速率 - I.依赖形态和峰值磁通量
The rotation rate of solar active and ephemeral regions -- I. Dependence on morphology and peak magnetic flux
论文作者
论文摘要
使用Helioseiscic和磁成像仪在船上获得的磁场图，我们测量了2010年至2016年之间观察到的864个活动速率和322个短暂区域的旋转速率。我们发现，与较大的磁性示踪剂相比，我们发现较小的磁性示踪剂显示出更快的旋转趋势。因此，短暂区域平均表现出最快的旋转速率。我们将活动区域进一步分为三个类。 A类包括磁性双梁，遵守Hale的极性定律，Joy的定律，与以下一项相比表现出更连贯的领先极性。第二类B级包括违反上述经验定律之一的活跃地区。第三类U组成了单极活动区域。我们发现A类和B类活性区域的旋转速率之间没有显着差异。相比之下，平均旋转速率平均表现出单极活性区域，旋转速率差异的分布较窄。假设旋转速率指示对流区域内磁性结构的锚定深度，我们认为A类和B类的活动区域可能固定在整个对流的信封中，而单极的单极活动区域则是植根于对流区域附近或浅层近距离深度深度深处的薄层中的一个根部的薄层。
Using magnetic field maps acquired by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory we measured rotation rates of 864 active and 322 ephemeral regions observed between 2010 and 2016. We found smaller magnetic tracers to show a tendency to rotate faster as compared to larger ones. Thus, ephemeral regions exhibit on average the fastest rotation rate. We further divided active regions into three classes. Class A comprised magnetic bipoles obeying Hale's polarity law, Joy's law, and exhibiting more coherent leading polarity in comparison with the following one. The second class B included active regions violating at least one of the aforementioned empirical laws. The third class U comprised unipolar active regions. We found no significant difference between the rotation rates of active regions of classes A and B. In contrast, unipolar active regions exhibited on average lower rotation rate and narrower distribution of the rotation rate differences. Assuming the rotation rate to indicate the anchoring depth of the magnetic structure within the convection zone, we supposed that active regions of classes A and B might be anchored throughout the entire convective envelope while unipolar active regions a rooted within a thin layer located either near the base of the convection zone or at a shallow near-surface depth.
