A 3D MHD simulation to model the dynamics of a pseudo-streamer

Understanding the physical mechanism responsible for the solar wind generation is one of the key objectives of Solar Orbiter. One of the existing theories to explain the observed properties of the slow wind is that the plasma, confined low in the solar atmosphere in closed magnetic field, is dynamically released into the open field thanks to magnetic reconnections between open and closed magnetic field. Although the local magnetic field properties has been frequently studied using static models, the dynamic of the open-closed magnetic boundary remains ill-understood. Our objective is to study the dynamics of specific magnetic geometries, pseudo-streamers, that can generate slow solar wind. We aim to perform 3D magnetohydrodynamics (MHD) numerical simulations of the solar corona and inner heliosphere using a MHD code with adaptive mesh refinement. We aim to model the dynamics of the open-closed coronal magnetic field using a 3D MHD code (ARMS) to study its role in the slow wind generation process