  During the Parker Solar Probe's (PSP) first perihelion pass, the spacecraft
reached within a heliocentric distance of \(\sim 37~R_\odot\) and observed
numerous magnetic and flow structures characterized by sharp gradients. To
better understand these intermittent structures in the young solar wind, an
important property to examine is their degree of correlation in time and space.
To this end, we use the well-tested Partial Variance of Increments (PVI)
technique to identify intermittent events in FIELDS and SWEAP observations of
magnetic and proton-velocity fields (respectively) during PSP's first solar
encounter, when the spacecraft was within 0.25 au from the Sun. We then examine
distributions of waiting times between events with varying separation and PVI
thresholds. We find power-law distributions for waiting times shorter than a
characteristic scale comparable to the correlation time, suggesting a high
degree of correlation that may originate in a clustering process. Waiting times
longer than this characteristic time are better described by an exponential,
suggesting a random memory-less Poisson process at play. These findings are
consistent with near-Earth observations of solar wind turbulence. The present
study complements the one by Dudok de Wit et al. (2020, present volume), which
focuses on waiting times between observed "switchbacks" in the radial magnetic
field.
