The MagnetoSheath Transport: From Local Kinetics to Global Dynamics (MAST) project quantitatively assesses the solar wind–magnetosphere–ionosphere (SW-M-I) energetics including effects of solar wind and magnetosheath fluctuations to resolve the energy dissipation processes and paths under a variety of solar wind and IMF conditions. Specifically, we seek to understand the solar wind energy entry processes through the magnetopause, and the effects of solar wind and/or magnetosheath fluctuations on these processes.

The research employs three global magnetospheric simulation setups employing two versions of the Space Weather Modeling Framework (SWMF) Geospace model and the Vlasiator global Vlasov simulation (collaboration with University of Helsinki). We  study the effects of kinetic processes by comparing the results between the models.

We   compare the model results with in-situ measurements using THEMIS, Van Allen Probes, MMS, Cluster, and other available spacecraft as well as with geomagnetic indices AU/AL and SYM-H, or their equivalents using additional stations provided by the SuperMAG network. We compare the energy dissipation in the ionosphere and in the inner magnetosphere using observational proxies based on the geomagnetic indices.

The MAST project falls under two research themes in our group: