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We use \emph{Parker Solar Probe} (\emph{PSP}) in-situ measurements to analyzethe characteristics of solar wind turbulence during the first solar encountercovering radial distances between $35.7R_\odot$ and $41.7R_\odot$. In ouranalysis we isolate so-called switchback (SB) intervals (folded magnetic fieldlines) from non-switchback (NSB) intervals, which mainly follow the Parkerspiral field. Using a technique based on conditioned correlation functions, weestimate the power spectra of Elsasser, magnetic and bulk velocity fieldsseparately in the SB and NSB intervals. In comparing the turbulent energyspectra of the two types of intervals, we find the following characteristics:1) The decorrelation length of the backward-propagating Elsasser field $z^-$ islarger in the NSB intervals than the one in the SB intervals; 2) the magneticpower spectrum in SB intervals is steeper, with spectral index close to -5/3,than in NSB intervals, which have a spectral index close to -3/2; 3) both SBand NSB turbulence are imbalanced with NSB having the largest cross-helicity,4) the residual energy is larger in the SB intervals than in NSB, and 5) theanalyzed fluctuations are dominated by Alfv\'enic fluctuations that arepropagating in the \emph{sunward} (\emph{anti-sunward}) direction for the SB(NSB) turbulence. These observed features provide further evidence that theswitchbacks observed by \emph{PSP} are associated with folded magnetic fieldlines giving insight into their turbulence nature.

Turbulence characteristics of switchbacks and non-switchbacks intervals observed by \emph{Parker Solar Probe}