Characterizing Solar Wind Variations and Solar Wind Source Regions using In-Situ Measurements and Modeling

The near-Sun environment and solar wind dynamics hold key insights into the Sun’s influence on our solar system. We harness the power of novel in-situ measurements of magnetic and electric fields, particles, and ions from the Parker Solar Probe (PSP) and Solar Orbiter (SO), to gain a comprehensive understanding of the complexities of the near-Sun environment. Our investigation involves combining data from PSP, SO, and magnetograms obtained from the Solar Dynamics Observatory Helioseismic and Magnetic Imager (SDO/HMI) and Global Oscillation Network Group (GONG) to discern and characterize the solar wind originating from distinct coronal source regions. Using Potential Field Source Surface (PFSS) and Magnetohydrodynamic (MHD) modeling, we identify the source region of the fast solar wind as coronal holes and slow solar wind as originating from active regions and coronal hole boundaries. We then combine these modeling efforts with in-situ observations to discern the variations in properties between solar wind emanating from coronal holes, coronal hole boundaries, and active regions, thereby facilitating a more comprehensive characterization of these phenomena. We focus on regions of enhancements in low first ionization potential (FIP) elements and particle density, as these variations provide crucial insights into the origin and nature of the solar wind. Our study uncovers a notable enhancement in low FIP elements over a pseudostreamer, offering valuable insights into the unique characteristics of these regions. This comprehensive analysis enables us to characterize the differences in elemental composition, particle density, and other relevant parameters, shedding light on the underlying mechanisms driving these phenomena.