3D non-adiabatic MHD simulation of solar prominence oscillations and eruption

Solar promineces, also known as solar filaments, are cloud-like cool and dense condensations floating in the hot and tenuous solar corona, the outmost layer of the solar atmosphere. Scientists show great interests in their formation, oscillation and eruption. Among the frequently observed oscillations, large-amplitude oscillations, whose typical velocity is over 20 km/s attract more and more studies, because they can provide vital information on the triggering process, restoring force and damping mechanisms in the solar corona. Moreover, some decayless oscillations are considered as the precursor for filament eruptions. The relationship between oscillations and eruptions is a hotly debated topic, yet poorly understood. Numerical simulation is in demand. In this proposal, we setup a plan to do a series 3D non-adiabatic simulations, from prominence oscillation to prominence eruption. The results are expected to help us have a better understanding of wave mode conversion, and non force free effects in the solar corona.