Evolution of Coronal Mass Ejections in the Solar Wind using Data-Driven Numerical Models

Numerical modeling of the solar wind and Coronal Mass Ejections (CMEs) is a vital tool for both space weather predictions as well as improving the understanding of CME evolution in the solar wind. We utilize the state-of-the-art 3D MHD model - Alfven Wave Solar atmosphere Model (AWSoM) and a self-consistent CME model - STITCH (Statistical Injection of Helicity Condensation) to simulate the global background solar wind plasma and initiate a CME eruption on the Sun. The STITCH method forms sheared arcades through helicity injection driven purely by photospheric magnetic field observations. These models are utilized to perform a detailed study of the structure and evolution of a CME propagating in the solar wind from the Sun to the Earth using 3D simulation results to probe multiple viewpoints in the corona and the inner heliosphere.