Thursday

One of the key goals of Solar Orbiter is to link in-situ and remote sensing data in order to study the connection between the inner solar atmosphere and the solar wind. With this regard, it will be crucial to have accurate and precise reconstructions of the solar magnetic field in order to identify which location on the solar surface the location of the spacecraft is connected to.
A number of force-free models have been put forward and these will probably address this challenge for most of the observational time, i.e. when the solar corona slowly evolves.
At the same time, as some observational campaigns will focus on solar eruptions and coronal mass ejections, it is key to understand how this connectivity changes during these violent and disruptive events when most of the force-free field assumptions stop being valid.
We will present a global MHD simulations of a study case, the CME from Dec, 30th 2014. In this work, we use a snapshot of a global magnetofrictional simulation as the eruptive initial condition of a MHD simulation that covers the whole solar corona until 4 Rsun. We find that the simulation reproduces most of the observable features and we address how the magnetic field connectivity between the external boundary of the MHD simulation and the solar surface is affected by the CME propagation.