We investigate the orientation of the photospheric magnetic fields in the solar polar region using observations from the Helioseismic and Magnetic Imager (HMI). Inside small patches of significant polarization, the inferred magnetic field vectors at 1″ scale appear to systematically deviate from the radial direction. Most tilt toward the pole; all are more inclined toward the plane of sky compared to the radial vector. These results, however, depend on the “filling factor” f that characterizes the unresolved magnetic structures. The default, uninformative f ≡ 1 for HMI will incur larger inclination and less radial fields than f < 1. The observed trend may be a systematic bias inherent to the limited resolution.

我们使用来自日震和磁成像仪 (HMI) 的观测来研究太阳极区中光球磁场的方向。在显着极化的小块内，推断的 1 英寸尺度的磁场矢量似乎系统地偏离了径向方向。大多数向极点倾斜；与径向矢量相比，所有这些都更倾向于天空平面。然而，这些结果取决于表征未分辨磁性结构的“填充因子” f 。HMI的默认、无信息f  ≡ 1 将产生比f  < 1 更大的倾角和更少的径向场。观察到的趋势可能是有限分辨率固有的系统偏差。