We propose to conduct global MHD simulations of the whole Solar convection zone. This first-of-a-kind simulation will connect internal dynamo simulations to the surface of the Sun on a global scale.
We will tackle highly disparate spatial and temporal scales, detailed microphysics, interplay between local and global effects, wide dynamic range, and required resolution in both space and time to resolve features at different depths of the atmosphere.
By using the speed and flexibility advantages offered by the DISPATCH code framework, we will be able to cover the tremendous range of scales and connect the magnetic dynamo to the photosphere of the Sun, which will give us insight into the convective conundrum, spot-dynamo paradox, flux emergence, etc.
We will start the simulations from our pilot LUMI-C run with 500 km resolution near the top boundary (Popovas et al., 2022). The run will continue for several convective turnover times before we will boost the resolution to 62.5 km by using static mesh refinement.
Lastly, we will extend the simulation slightly beyond the photosphere. The relaxation will need 96 nodes per job for continuous use and the last step will need 486 nodes, so LUMI-C is perfect for this project.