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The Sun's corona, heated to temperatures exceeding one million Kelvin despitelying above the cooler photosphere, has puzzled astrophysicists since itsdiscovery in the 1940s. Prevailing theories, based on acoustic andmagnetohydrodynamic waves, and micro/nano-flares, fail to fully account forthis extreme heating or the origins of the supersonic solar wind. We propose amechanism in which magnetic reconnection rapidly reconfigures field lines andexerts a torque on the magnetic moment of gyrating charged particles. Thistorque transfers magnetic energy to the particles, effectively doubling theirenergy and heating the plasma. As particles traverse multiple reconnectionsites, they gradually heat to coronal temperatures. With just a few additionalcrossings, particles can gain enough energy to overcome the Sun's gravity,directly driving solar wind acceleration. Our hypothesis resolves the coronalheating paradox and unifies solar wind dynamics under a universal astrophysicalprocess. This work redefines our understanding of energy transfer in magnetizedplasmas, with implications extending to stellar and astrophysical systems.

The Solar Enigma Decoding the Mystery of the Hot Corona and Solar Wind Acceleration