  Using a classification scheme for solar wind type based on the heliocentric
distance of the observation, we look at near perihelion observations from
Parker Solar Probe Encounters Four to Fourteen to study the sources of the slow
Alfvenic solar wind (SASW). Through Potential Field Source Surface (PFSS)
modeling and ballistic mapping, we connect streams to their solar source and
find that a primary population of SASW comes from small coronal holes (CHs) and
their over-expanded boundaries, while a second population seems to emerge from
non-CH structures potentially through interchange reconnection with nearby open
field lines. This CH-like SASW shows larger expansion than the FSW, potentially
indicating additional heating below the critical point leading to slower wind
emerging from CH-like structures. We show that SASW emerging from CH-like
structures shows stronger preferential acceleration of alpha particles (similar
to the FSW) than the SASW emerging from non-CH structures, and that this is a
velocity dependent phenomena as found in previous studies. To have additional
confidence in our mapping results, we quantify the error on both the PFSS model
and ballistic mapping and discuss how additional multi-point observations of
plasma parameters and composition would allow us to better constrain our models
and connect the solar wind to its source.
