Speaker
Description
Magnetohydrodynamic modelling of the evolution and dynamics of large-scale heliospheric disturbances is conventionally carried out employing either a coronal or heliospheric approach. In the former, the complex dynamics from the low corona to the heliosphere is modeled, while in the latter the simulation is started at heliocentric distances at which the solar wind is characterised by super-Alfvénic outflow. We have developed a best-of-both-worlds alternative to this paradigm, wherein the middle corona is included in the model, encompassing a spatial domain starting at ~3-5 solar radii and extending out to the heliosphere. In this work, we focus on our efforts to evaluate the performance of the model using multi-spacecraft observations, and discuss the path towards using the model for operational space weather predictions.
