Authors: Tamar Ervin (Space Sciences Laboratory | UC Berkeley), Stuart D. Bale (Space Sciences Laboratory | UC Berkeley), Samuel Badman (Center for Astrophysics | Harvard & Smithsonian), Pete Riley (Predictive Science Inc.), Yeimy Rivera (Center for Astrophysics | Harvard & Smithsonian)

The use of multi-spacecraft radial alignments allow us to study plasma packets measured by a variety of instruments on these spacecraft. Using a combination of data from Parker Solar Probe (PSP), Solar Orbiter (SO), and magnetograms from the Solar Dynamics Observatory Helioseismic and Magnetic Imager (SDO/HMI) and Global Oscillation Network Group (GONG), we look at enhancements in particle density and low first ionization potential (FIP) elements to characterize the solar wind originating from coronal holes, coronal hole boundaries, and active regions. Using PFSS and MHD modeling, we identify fast wind originating from coronal holes and slow wind from multiple source regions (coronal hole boundaries and active regions). This is supported by observations of both helium-rich and helium-poor slow solar wind plasma along with variance in the normalized Fe/O abundance ratio over the encounter thus implying multiple origin regions of the slow solar wind.