The dynamics of solar prominences

Solar prominences (so called when observe above the solar limb. When they are observed on the solar disk, they are called filaments) can be stable for weeks. However, when they erupt, coronal mass ejections will often be produced. The mechanisms that trigger the eruptions are being debated by researchers, and so are the structures and dynamics of prominences. The thesis will utilize data from Solar Dynamics Observatory, which has superb spatial and temporal resolutions of the sun. The thesis will conduct multi-wavelength analysis of the thermodynamics of solar prominences, the connection between prominences' magnetic field and the surrounding coronal cavity, and the interaction between prominences with their surrounding corona through MHD instabilities.