Switchbacks are widely acknowledged phenomena observed by the Parker Solar Probe and appear to occur in patches. Previous studies focused on the fluctuations at the magnetic reversals. However, the nature of the fluctuations inside the switchbacks remains unknown. Here we utilize the magnetic field data and plasma data measured by the Parker Solar Probe in the first four encounters. We investigate the fluctuations in the switchback intervals of 100 s with at every instant and compare them to the fluctuations in the nonswitchback intervals of 100 s with at every instant. We calculate normalized cross-helicity , normalized residual energy , correlation coefficient C _vb between and , Alfvn ratio r _A, and the amplitude of magnetic and kinetic fluctuations. We find that the switchback intervals exhibit a distribution of similar with the nonswitchback intervals. However, the r _A of switchback intervals is around 0.35, while the nonswitchback intervals have r _A around 0.65, indicating the fluctuations in the switchbacks are more magnetically dominated. We also find that the distribution pattern of pixel average amplitude of both and of switchback intervals in the C _vb– plane show a vertical stripe feature at , illustrating the possible magnetically dominant magnetic-velocity alignment structure. These results will help us to understand the nature and the formation of the switchback turbulence.

折返是帕克太阳探测器观察到的广泛公认的现象，并且似乎以补丁形式出现。以前的研究集中在磁反转的波动上。然而，折返线内部波动的性质仍然未知。在这里，我们利用了帕克太阳探测器在前四次遭遇中测量的磁场数据和等离子体数据。我们调查了每瞬间100 秒的切回间隔的波动，并将它们与每瞬间100 秒的非切回间隔的波动进行比较。我们计算归一化交叉螺旋度、归一化残余能量、和之间的相关系数C _vb、Alfvn 比值r _A，以及磁和动力学波动的幅度。我们发现折返间隔表现出与非折返间隔相似的分布。然而，折返区间的r _A约为 0.35，而非折返区间的r _A约为 0.65，表明折返区间的波动更受磁力支配。我们还发现，C _vb –平面中和折返间隔的像素平均幅度的分布模式在 ，说明可能的磁主导磁速排列结构。这些结果将有助于我们了解折返湍流的性质和形成。