Speaker
Description
The coronal heating problem remains a central challenge in solar physics, which requires a detailed understanding of wave-based heating mechanisms. While the Alfvén Wave Solar Model (AWSoM) has shown great success in physics-based modelling of the solar corona, its focus on a single heating mechanism leaves room for improvement. This is why we developed the Uniturbulence and Alfvén Wave Solar Model (UAWSoM), which additionally includes heating due to uniturbulent kink wave dissipation. We constructed the theoretical framework necessary to derive the governing kink wave energy evolution equations. This was followed by implementing a 1D version of the model in MPI-AMRVAC, where we showed that kink waves are able to sustain a stable coronal atmosphere without requiring an artificial background heating term. We found that kink wave dissipation is more efficient at heating the lower corona than Alfvén wave dissipation and its inclusion improves model stability. Further, we demonstrate the usage of UAWSoM in 1D coronal loop modelling and compare the results with other analytical and numerical methods. Finally, we present the ongoing efforts, focusing on the development of the 3D version of the model. We envision that the resulting self-consistent 3D coronal model will offer a lot of potential for space weather modelling.
| Numerical model | UAWSoM |
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