Mathematical modelling of MHD instabilities in solar jet structures

working on observational, numerical and analytical studies of the Kelvin-Helmholtz and Rayleigh-Taylor in solar plasma. In particular:
- observationally identify regimes of appearance of the RT instability, its morphology and lifetime by analysing Solar Optical Telescope data (Ca II spectral lines) on board the Hinode satellite and ground-based data from the Swedish Solar Telescope (SST).
- numerically model jet like structures, with particular interest in processes related to the magnetic field strength and direction to analyse the appearance and development of the RT instability at the top part of the jet due-to effective acceleration. Additionally, investigate processes related to the Kelvin-Helmholtz (KH) instability taking place during the evolution of the jet.
- analytically obtain conditions for RT and KH instabilities in the presence of a magnetic field (for example modeled by using self-similar approach) and apply them to the observational and numerical data discussed in the previous points.
- analysis of wave excitation (MHD waves including Alfven) and their energy budget directly due to jet propagation.