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Switchbacks are widely acknowledged phenomena observed by the Parker SolarProbe and appear to occur in patches. Previous studies focused on thefluctuations at the magnetic reversals. However, the nature of the fluctuationsinside the switchbacks remains unknown. Here we utilize the magnetic field dataand plasma data measured by the Parker Solar Probe in the first fourencounters. We investigate the fluctuations in the switchback intervals of 100s with BR>0 at every instant and compare them to the fluctuations in thenonswitchback intervals of 100 s with theta_RB>160o at every instant. Wecalculate normalized cross-helicity sigma_c, normalized residual energysigma_r, correlation coefficient C_vb between dvA and dv, Alfven ratio rA, andthe amplitude of magnetic and kinetic fluctuations. We find that the switchbackintervals exhibit a distribution of sigma_c similar with the nonswitchbackintervals. However, the rA of switchback intervals is around 0.35, while thenonswitchback intervals have rA around 0.65, indicating the fluctuations in theswitchbacks are more magnetically dominated. We also find that the distributionpattern of pixel average amplitude of both dvA and dv of switchback intervalsin the C_vb-sigma_r plane show a vertical stripe feature at C_vb>0.8,illustrating the possible magnetically dominant magnetic-velocity alignmentstructure. These results will help us to understand the nature and theformation of the switchback turbulence.

Large Amplitude Switchback Turbulence: Possible Magnetic Velocity Alignment Structures