  The solar wind undergoes significant heating as it propagates away from the
Sun; the exact mechanisms responsible for this heating remain unclear. Using
data from the first perihelion of the Parker Solar Probe mission, we examine
the properties of proton and electron heating occurring within magnetic
coherent structures identified by means of the Partial Variance of Increments
(PVI) method. Statistically, regions of space with strong gradients in the
magnetic field, $PVI \geq 1$, are associated with strongly enhanced proton but
only slightly elevated electron temperatures. Our analysis indicates a heating
mechanism in the nascent solar wind environment facilitated by a nonlinear
turbulent cascade that preferentially heats protons over electrons.
