Statistical relationships between solar wind parameters and ion precipitation fluxes across all extreme events. The figure consists of six panels arranged in three rows: (a) low-energy ion precipitation flux (30–650 eV) expressed as ﹩\mathrm{ln}(1+F)﹩ versus solar wind dynamic pressure P_dyn; (b) high-energy ion precipitation flux (650–25,000 eV) ﹩\mathrm{ln}(1+F)﹩ versus P_dyn; (c) ﹩\mathrm{ln}(1+F)﹩ for low-energy ions versus ∣B∣; (d) ﹩\mathrm{ln}(1+F)﹩ for high-energy ions versus ∣B∣; (e) ﹩\mathrm{ln}(1+F)﹩ for low-energy ions versus M_A; (f) ﹩\mathrm{ln}(1+F)﹩ for high-energy ions versus M_A. The scatter plots (dots) display median-based event data, and solid (or dashed) lines indicate the fitted trends. We plot precipitation fluxes as ﹩\mathrm{ln}(1+F)﹩ to compress the large dynamic range, reduce skewness and the influence of extreme values, and to ensure the quantity is defined when F = 0.