| 4/20 |
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Denis |
Acceleration process of a solar filament eruption: observation and numerical modeling |
In this talk, I will explore the dynamics and acceleration process of a fast-filament eruption by combining imaging spectroscopy observations and numerical modeling.
By adapting the toroidal current loop equations within the context of the torus instability, we modeled the evolution of the filament eruption and solved the equation of motion for different scenarios involving full and partial toroidal flux rope configurations.
We demonstrate that the eruption process of the filament can be equally described by models based on either the conservation of magnetic flux or conservation of total energy, with the added constraint that the electric current accounting for the free magnetic energy is restricted to the expanding flux rope above the photosphere.
However, neither model independently satisfies the conservation of energy and magnetic flux simultaneously.
We propose a novel composite model that incorporates a non-constant aspect ratio for the toroidal flux rope.
This composite model not only maintains consistency with the conservation laws but also yields a remarkable fit to the observational data, thus offering a more comprehensive representation of the eruption process.
Furthermore, by incorporating the mass-loss effect in our simulations, we successfully reproduced the fast component of the eruption. This confirms that mass loss, manifesting as draining material or downflows, directly modulates the acceleration phase of the filament.
Based on the results of our best-fitting model, we also quantified the energy budget of the high-speed eruption.
Additionally, the role of the driving forces in the evolution of the toroidal flux rope is also investigated.
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