  We use data from the first six encounters of Parker Solar Probe and employ
the Partial Variance of Increments ($PVI$) method to study the statistical
properties of coherent structures in the inner heliosphere with the aim of
exploring physical connections between magnetic field intermittency and
observable consequences such as plasma heating and turbulence dissipation. Our
results support proton heating localized in the vicinity of, and strongly
correlated with, magnetic structures characterized by $PVI \geq 1$. We show
that on average, such events constitute $\approx 19\%$ of the dataset, though
variations may occur depending on the plasma parameters. We show that the
waiting time distribution ($WT$) of identified events is consistent across all
six encounters following a power-law scaling at lower $WTs$. This result
indicates that coherent structures are not evenly distributed in the solar wind
but rather tend to be tightly correlated and form clusters. We observe that the
strongest magnetic discontinuities, $PVI \geq 6$, usually associated with
reconnection exhausts, are sites where magnetic energy is locally dissipated in
proton heating and are associated with the most abrupt changes in proton
temperature. However, due to the scarcity of such events, their relative
contribution to energy dissipation is minor. Taking clustering effects into
consideration, we show that smaller scale, more frequent structures with PVI
between, $1\lesssim PVI \lesssim 6$, play the major role in magnetic energy
dissipation. The number density of such events is strongly associated with the
global solar wind temperature, with denser intervals being associated with
higher $T_{p}$.
