The reversal of the solar polar magnetic fields
The reversal of the solar polar magnetic fields
复制标题
太阳极地磁场的逆转
DOI：
10.1007/bf00146532
复制
发表时间：
1991
期刊：
影响因子：
2.8
通讯作者：
P. McIntosh
中科院分区：
文献类型：
--
作者：
P. R. Wilson;P. McIntosh
利用国家太阳观测站提供的天气磁数据和根据威尔逊山太阳观测站提供的数据绘制的等高线图，对1986年太阳黑子极小期（第22周开始）附近的第一次大规模磁场模式进行了观测。后者进行了比较模拟等值线图来自磁通量输运方程的数值解，使用特定的卡林顿旋转的数据作为初始条件。模拟的大尺度磁场的演变与观测到的演变定性一致，但在几个重要的方面有所不同。通过改变扩散率和大尺度速度场的参数，可以消除一些差异。其余的差异包括：（i）精细结构的复杂性，（ii）对差异旋转的响应，（iii）衰减活动区的演化，（iv）与观测活动区演化无关的弱大尺度磁场中新元素的出现，从而得出结论：构成大尺度特征的弱磁场图案不能完全由活动区的扩散衰减形成。必须有一个显着的贡献，这些模式的网络结构内的非随机流量爆发，独立的活动区域。
Observations of the first large-scale patterns of magnetic fields near the sunspot minimum of 1986 (the start of cycle 22) are presented using synoptic magnetic data provided by the National Solar Observatory and contour maps constructed from data provided by the Mount Wilson Solar Observatory. The latter are compared with simulated contour maps derived from numerical solutions of the flux transport equation using data from particular Carrington rotations as initial conditions.The simulated evolutions of the large-scale magnetic fields are qualitatively consistent with observed evolutions, but differ in several significant respects. Some of the differences can be removed by varying the diffusivity and the parameters of the large-scale velocity fields. The remaining differences include: (i) the complexity of fine structure, (ii) the response to differential rotation, (iii) the evolution of decaying active regions, and (iv) the emergence of new elements in the weak, large-scale fields independent of the evolution of the observed active regions.It is concluded that the patterns of weak magnetic fields which comprise the large-scale features cannot be formed entirely by the diffusive decay of active regions. There must be a significant contribution to these patterns by non-random flux eruptions within the network structure, independent of active regions.