  Parker Solar Probes's (PSP)'s unique orbital path allows us to observe the
solar wind closer to the Sun than ever before. Essential to advancing our
knowledge of solar wind and energetic particle formation is identifying the
sources of PSP observations. We report on results for the first two PSP solar
encounters derived using the Wang-Sheeley-Arge (WSA) model driven by Air Force
Data Assimilative Photospheric Flux Transport (ADAPT) model maps. We derive the
coronal magnetic field and the 1 Rs source regions of the PSP-observed solar
wind. We validate our results with the solar wind speed and magnetic polarity
observed at PSP. When modeling results are very reliable, we derive time series
of model-derived spacecraft separation from the heliospheric current sheet,
magnetic expansion factor, coronal hole boundary distance, and photospheric
field strength along the field lines estimated to be connected to the
spacecraft. We present new results for Encounter 1, which show time evolution
of the far-side mid-latitude coronal hole that PSP co-rotates with. We discuss
how this evolution coincides with solar wind speed, density, and temperature
observed at the spacecraft. During Encounter 2, a new active region emerges on
the far-side, making it difficult to model. We show that ADAPT-WSA output
agrees well with PSP observations once this active region rotates onto the
near-side, allowing us to reliably estimate the solar wind sources
retrospectively for most of the encounter. We close with ways in which coronal
modeling enables scientific interpretation of these encounters that would
otherwise not have been possible.
