Authors: Chip Manchester (University of Michigan), Nishtha Sachdeva (University of Michigan), Zhenguang Huang (University of Michigan), Igor Sokolov (University of Michigan), Jia Huang (University of California, Berkeley), Lulu Zhao (University of Michigan)
We simulate the solar wind including CMEs during the PSP era including the September 05, 2022 (Labor Day) CME Event from eruption to interplanetary propagation with the Alfven Wave Solar Model (AWSoM). The model includes energy partitioning between parallel and perpendicular proton and isotropic electron temperature. This fast CME was well observed by Parker Solar Probe (PSP) and Solar Orbiter (SOLO) with both remote and in situ instruments providing unprecedented wealth of information of the CME’s structure and evolution. With an average transit speed of roughly 2000 km/s, the CME produced a wide range of disturbances in the corona and heliosphere including intense solar energetic particles. We begin by simulating with SOLO/Extreme Ultraviolet Imager (EUI) data to characterize the pre-eruption state of this far-side event. CME simulation results are compared with situ observations from the SOLO Solar Wind Plasma Analyzer (SWA), both ion sensors and electron analyzer and data from the PSP/Solar Wind Electrons Alphas and Protons (SWEAP) instrument and the PSP/FIELDS instrument. This wealth of data, we compare simulation results to the large-scale plasma distribution and magnetic fields structure of the CME as well as the detailed state of the entrained plasma including isotropic electron temperature, anisotropic proton temperature and turbulent energy density. All combined, model and data provide a broad view of the detailed CME plasma structure and its interaction with Alfvenic turbulence.