  A variety of energy sources, ranging from dynamic processes like magnetic
reconnection and waves to quasi-steady terms like the plasma pressure, may
contribute to the acceleration of the solar wind. We utilize a combination of
charged particle and magnetic field observations from the Parker Solar Probe
(PSP) to attempt to quantify the steady-state contribution of the proton
pressure, the electric potential, and the wave energy to the solar wind proton
acceleration observed by PSP between 13.3 and ~100 solar radii (RS). The proton
pressure provides a natural kinematic driver of the outflow. The ambipolar
electric potential acts to couple the electron pressure to the protons,
providing another definite proton acceleration term. Fluctuations and waves,
while inherently dynamic, can act as an additional effective steady-state
pressure term. To analyze the contributions of these terms, we utilize radial
binning of single-point PSP measurements, as well as repeated crossings of the
same stream at different distances on individual PSP orbits (i.e. "fast radial
scans"). In agreement with previous work, we find that the electric potential
contains sufficient energy to fully explain the acceleration of the slower wind
streams. On the other hand, we find that the wave pressure plays an
increasingly important role in the faster wind streams. The combination of
these terms can explain the continuing acceleration of both slow and fast wind
streams beyond 13.3 RS.
