Authors: Liang Zhao (U. of Michigan), Susan T. Lepri (U. of Michigan), Enrico Landi (U. of Michigan), Jackson R. MacTaggart (U. of Michigan), Catherine Ballard (U. of Michigan), and Henry Han (Balor University)

We analyze long-term observations of solar wind in-situ properties from ACE/SWICS and SWEPAM, along with coronal EUV images from SOHO/EIT, STEREO/SECCHI, and SDO/AIA, during Solar Cycles 23–25. Different coronal structures—such as Active Regions (ARs), Low-latitude Coronal Holes (LCHs), Polar Coronal Holes (PCHs), and Quiet Sun (QS) regions—are identified using pixel values from the EUV synoptic images. We address the space-weather-induced degradation of the ACE/SWICS instrument and introduce a method to minimize its impact. As an example, we demonstrate how the post-degradation SWICS 2.0 heavy ion composition data can be used to analyze streamer-associated solar wind. We then compare coronal structures and solar wind in-situ properties during the ascending phases of the three most recent solar cycles. We find that Cycle 23 has the largest AR and PCH regions but the smallest LCH region; Cycle 24 has the smallest AR and PCH areas; and Cycle 25 shows the largest LCH region. The trends in AR and PCH regions align with the solar cycle strength, as indicated by the monthly sunspot number. In addition, the proton speed, density, O⁷⁺/O⁶⁺ ratio, and Fe/O ratio of streamer-associated solar wind all follow the trends of sunspot number, AR, and PCH areas across the three cycles. We conclude that solar wind in-situ properties closely reflect changes in the solar corona.