From Flare to Tornado: Tracing Energy Propagation in the Solar Atmosphere

Defining the mechanisms that describe how energy propagates through the solar atmosphere remains a central challenge in solar physics. This study investigates a class X1.9 solar flare using high-cadence multiwavelength imaging data from the Dunn Solar Telescope's (DST) Zyla Hydrogen-Alpha Rapid Dynamics Camera (HARDcam), Rapid Oscillations in the Solar Atmosphere (ROSA), and the Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA), and Helioseismic and Magnetic Imager (HMI). This X1.9 flare triggered a cascade of solar phenomena including Hard X-ray jets, multiple smaller flares, and swirl-driven coronal heating creating a magnetic energy induced solar tornado eruption. Through multiwavelength light curve analysis, empirical mode decomposition, and differential emission measure using a regularized inversion method (DEMReg) we search for quasi-periodic pulsations (QPP) and identify the flare properties, morphology, velocities, energy release, and temperatures. These findings signal a link between QPP behavior and the onset of complex eruptive events, providing new insights into the mechanisms of energy release and transport in the solar atmosphere.