Abstract:This study presents experimental evidence of a non-linear energy cascade and high-frequency magnetic oscillations in the middle solar corona, identified through a novel analytical approach termed the KM Model. Utilizing high-cadence (5-second) L2 sequential data from the ASPIICS coronagraph, we analyze the radial evolution of dominant oscillation periods across four cardinal sectors during two distinct epochs (September and October 2025). Our findings reveal a characteristic "U-shaped" frequency profile. In the "Magnetic Filter" zone (approx. 1.5 Rs), we identify a stabilization of low-frequency modes (periods of 98–120 s). This is followed by a dramatic transition into the "Magnetic Shake" regime (1.5–1.8 Rs), where periods synchronously collapse to high-frequency modes ranging from 8.1 s to 15.4 s (approx. 65–123 mHz). The robustness of the KM Model is verified through a "Shuffle-and-Reconstruct" causality test involving over 100 frames, confirming that the detected signal reflects real temporal physical evolution rather than instrumental noise or static brightness. The invariance of the resonance nodes across a 27-day solar rotation cycle suggests a permanent resonant structure responsible for coronal heating via magnetic stress dissipation.