Fundamental physical processes governing energy storage, transport, and release in the solar atmosphere are expected to operate on extremely small spatial and temporal scales, often at or below the resolution achievable by most observatories. Recently, novel high-resolution observations from modern facilities—such as the Daniel K. Inouye Solar Telescope (DKIST), the Goode Solar Telescope (GST), Solar Orbiter etc. —have begun to provide crucial insight into the occurrence and properties of these processes. They include thermal instabilities that drive coronal rain and prominences, observations of magnetized Kelvin-Helmholtz instabilities in the photosphere and corona, and tearing instabilities and turbulence within current sheets, to name a few. Such high-resolution observations provide robust constraints against which modern MHD numerical simulations must be validated. 

In this session, we welcome studies exploring fine-scale structures and rapid dynamic processes in the solar atmosphere. Observational, modeling, and theoretical studies as well as developments in solar instrumentation are all encouraged.