  We consider the possibility that aeolian (wind blown) processes occur on
small, 1 to 100~km diameter, planetesimals when they were embedded in the
protosolar nebula. Drag from a headwind within a protostellar disk is
sufficiently large to loft cm and smaller sized particles off the surface of a
10 km diameter asteroid in the inner solar system (at a few AU), and micron
sized particles off the surface of a 10 km diameter object in the
Transneptunian region. The headwind is sufficiently strong to overcome surface
cohesion in the inner solar system, but not in the outer solar system. However,
in the outer solar system, surface particles can be redistributed or escape due
to impacts from particles that are in the protosolar disk's wind. Based on
scaling crater ejecta, we estimate that impacts from particles in the headwind
will lead to erosion of mass rather than accretion for planetesimals below
about 6 km in diameter. The erosion limit is independent of material strength
but proportional to the wind velocity. We explore the sensitivity of splash
particle trajectories to particle size, headwind velocity and Reynolds number.
Winds from a protostellar disk could account for Kuiper Belt Object (486958)
Arrokoth's smooth undulating terrain but only during an epoch of high particle
flux and low wind velocity. These conditions could have been present during and
just after coalescence of Arrokoth's building blocks.
