Numerical simulations of the formation and eruption of solar prominences

Prominences are one of the fascinating phenomena embedded in the solar atmosphere. Their temperature is significantly lower but the density is much higher than the surroundings. In addition, the prominence is an excellent indicator of the non-potential magnetic field, and their fine structures probably shed light on their supporting magnetic topological structures. Moreover, prominences are not always stable, and their eruptions are intimately related to solar flares and coronal mass ejections (CME), which can be linked by a standard flare model with magnetic reconnection. Thus, the studies about the formation and eruption of prominences not only enhance our understanding on the fundamental thermodynamic and magnetic-field evolution but also have significance for space weather forecasting. In this thesis, we study the whole life of the prominence with the aid of simulations, including the formation, eruption in the corona and CME propagation in the heliosphere. Concretely, we explore the potential relationships between filament fine structures and their magnetic structures. Secondly, we develop data-driven models to reproduce the formation and eruption of the flux rope, and analyze the magnetic reconnection and thermal process. Thirdly, we develop advanced data-driven flux rope models in EUHFORIA and COCONUT, and simulate the evolution of the flux rope in the heliosphere. We believe that this self-consistent and sun-to-earth simulation should be able to predict disastrous space weather events more accurately.