Description
Solar prominences are long, cool, dense features of the solar atmosphere. Within prominences, observations and simulations both show fine threadlike structures as mass collects within the magnetic dips. We study the formation and evolution of this mass falling under gravity beneath a dense prominence region through a less dense corona under the Magnetic Rayleigh-Taylor Instability (MRTI) in compressible and resistive 2.5D and 3D simulations using MPI-AMRVAC. We use high spatio-temporal resolution (order 10 km, 0.1 sec) to investigate the rise of secondary mixed-mode instabilities such as further Rayleigh-Taylor and Kelvin-Helmholtz instabilities along the leading edge of the falling RT knots, focussing on their initial descent through the corona. We compare the evolution of these secondary instabilities to mixing timescales and turbulent energy cascades across a range of field strengths and create synthetic observations to predict what can be seen by the Daniel K. Inouye Solar Telescope.
