Vol. 7, Issue 2, Part A (2025)

Auroral emissions occur as a result of the influx of high-energy electrons, as well as protons, which descend along the magnetic field lines, thereby infiltrating the Earth's atmospheric layers. Luminous and extensive auroras observed in the polar zones indicate perturbations within the magnetosphere and solar wind; such perturbations, in numerous cases, have the potential to forecast auroral phenomena. The depiction of the auroral oval serves as a critical indicator of space weather phenomena. A comprehensive 27-year investigation (spanning from 1 January 1997 to 20 July 2024) was undertaken focusing on various magnetic field and solar wind parameters—specifically, the interplanetary magnetic field, solar wind proton density, solar wind plasma flow velocity, flow pressure, among others—utilizing the KP index as a framework for analysis. The superposed epoch methodology is employed to analyze events classified as active and minor (G1), moderate (G2), strong (G3), severe (G4), and extreme (G5) storms, with Spearman’s rank correlation employed to demonstrate a monotonic relationship across all parameters investigated. The correlation observed between the rankings of the interplanetary magnetic field and the KP index registers at +0.9 during G2 and G3 storm events. Furthermore, the solar wind plasma velocity and flow pressure exhibit correlations of +0.8 and +0.7, respectively, concerning active and G1 storm classifications. This manuscript examines the intricacies of the Interplanetary Magnetic Field (IMF) in conjunction with the characteristics of solar wind, particularly regarding auroral phenomena and the interaction between solar wind and both the Earth and its magnetosphere.