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Transverse magnetohydrodynamic (MHD) waves have been shown to be ubiquitousin the solar atmosphere and can in principle carry sufficient energy togenerate and maintain the Sun's million-degree outer atmosphere or corona.However, direct evidence of the dissipation process of these waves andsubsequent heating has not yet been directly observed. Here we report on highspatial, temporal, and spectral resolution observations of a solar prominencethat show a compelling signature of so-called resonant absorption, a longhypothesized mechanism to efficiently convert and dissipate transverse waveenergy into heat. Aside from coherence in the transverse direction, ourobservations show telltale phase differences around 180 degrees betweentransverse motions in the plane-of-sky and line-of-sight velocities of theoscillating fine structures or threads, and also suggest significant heatingfrom chromospheric to higher temperatures. Comparison with advanced numericalsimulations support a scenario in which transverse oscillations trigger aKelvin-Helmholtz instability (KHI) at the boundaries of oscillating threads viaresonant absorption. This instability leads to numerous thin current sheets inwhich wave energy is dissipated and plasma is heated. Our results providedirect evidence for wave-related heating in action, one of the candidatecoronal heating mechanisms.

Resonant Absorption of Transverse Oscillations and Associated Heating in a Solar Prominence. I- Observational aspects