Parallel sessions

Understanding the physical mechanisms responsible for heating the solar corona remains an intriguing problem in solar physics. Observations suggest the presence of ubiquitous magnetic jets (e.g., spicules, fibrils, rapid blue/red-shifted excursions) in the chromosphere that topologically links the photosphere with the corona. These features not only transport mass, energy, and momentum across the transition region to balance the radiative and mass losses in the corona, but also accelerate the solar wind. Moreover, these structures act as conduits for magnetohydrodynamic (MHD) wave modes to propagate from the lower solar atmosphere to the corona and transfer energy between these regions. In recent years, the identification of dominant/linear MHD waves was reported via an interpretation of bulk motions of these jet structures in a simplified approximation. It must be noted that wave behaviour in the lower solar atmosphere is much more complicated due to the presence of linear/nonlinear/coupled wave modes that are subject to mode-conversion, phase mixing, instabilities, resonant absorption and ambipolar diffusion. While direct observations of these intricate mechanisms still remain a challenge to theorists and observers, it is now anticipated that high-resolution instrumentation, both in space (SDO, IRIS, Parker Solar Probe, Solar Orbiter) and ground (SST, GREGOR, BBSO), will aid researchers to gain an insight into the vital clues regarding energy transfer and dissipation mechanisms. Furthermore, the imminent commencing of the highest ever resolution, 4-metre-aperture solar telescope DKIST, will be a step-change in the understanding of unresolved plasma and MHD wave mechanisms that heat the corona and power the solar wind by providing an unprecedented spatial, temporal and spectral resolution. This session aims to bring together both theoretical (analytical and numerical) and observational aspects to discuss the recent advances in the field of MHD waves and magnetic jet structures in the lower solar atmosphere. The main goal of these sessions is to bring a synergy between international and UK researchers to identify pathways to explore key mechanisms associated with jets and MHD wave energy dissipation in context of upcoming observational facilities.