We combine global coronal models, in-situ observations of the solar wind, and remote observations of the solar atmosphere to trace and study the source region characteristics associated with highly Alfvénic solar wind observed through the inner heliosphere. We discuss a case study combining modeling and multipoint in-situ composition measurements to trace wind sources, finding that the Alfvénic streams of interest emerged from coronal hole boundaries. The slow Alfvénic wind stream of interest showed mixed elemental composition metrics, pointing to additional work being necessary to fully understand the source and emergence of these streams. Through studying additional near-Sun wind streams observed by Parker Solar Probe, we find that the majority of slow Alfvénic wind streams emerge from overexpanded boundaries of coronal hole structures. This wind is characterized by low magnetic field strength at the estimated footpoint, low mass flux, and large expansion factors consistent with coronal hole type structures. A second class of slow Alfvénic wind streams is found to emerge from regions with high footpoint field strength, high mass flux, and large expansion factors indicating large heating below the critical point in a hot structure. We discuss the necessity for full-Sun coverage of the solar magnetic field coupled with heavy ion diagnostics to fully close our understanding of solar wind sources and emergence mechanisms.