Magnetohydrodynamic wave interaction with flows in the Sun's chromosphere

The Sun is our nearest star with a direct impact on life and technology on Earth. Space-born and ground-based instruments have confirmed the ubiquitous presence of magnetohydrodynamic (MHD) waves throughout its atmosphere. They provide insight into the major unanswered questions of solar physics. MHD waves are capable of transferring energy and mechanical momentum from the convection zone into the corona and heliosphere. They are often associated with space weather activity such as solar flares and coronal mass ejections. Owing to the great success of MHD wave theory, we possess a diagnostic tool to extract detailed, local knowledge of physical conditions in the solar atmosphere. The UK, and the University of Warwick in particular, are internationally recognised leaders in this field. This project lends itself to a holistic approach that combines observational analysis, theoretical and numerical modelling.
With the recent inauguration of the new ground-based Daniel K. Inouye Solar Telescope (DKIST), with its unprecedented resolution, there is a renewed focus on chromospheric dynamics. This project will study the occurrence of MHD waves in chromospheric structures such as flare ribbons and swirls. Flare ribbons are chromospheric regions of heating due to magnetic reconnection events higher-up. They are accompanied by a variety of wave activity such as fast waves that ripple across ribbons as well as acoustic shocks propagating up. In particular, the project will focus on the role of inflows on the strength of wave dynamics and transport of energy and momentum into the upper chromosphere.