Numerical Modelling of Convection and Dynamo Processes in Fully Convective Stars
In the current project, we simulate thermal convection and generation of magnetic fields inside a fully convective star, like an M-dwarf or a T-tauri star. The numerical resolution required to reasonably well describe convection properties inside the star is 2563 to 5123.
KeywordsMagnetic Field Differential Rotation Meridional Circulation Protoplanetary Disc Stellar Surface
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