Authors: A.J. McCubbin (JHU APL), E. Provornikova (JHU APL), V.G. Merkin (JHU APL), S. Gibson (NCAR/HAO), N. Arge (NASA/GSFC)

Modern coronagraphs like WISPR on Parker Solar Probe and SoloHi on Solar Orbiter have revealed abundant fine structures in CMEs even at large distances from the Sun. These fine structures can originate from the complex internal dynamics during CME eruption in the corona or from interactions with structures in the surrounding solar wind. Aiming to untangle the details of remote CME observations, we present a GAMERA-Helio simulation, representing the highest resolution ever achieved in studying CMEs as they propagate through the inner heliosphere solar wind. This simulation resolves scales as small as ~10^5 km. Employing the analytical Gibson-Low CME model, we simulate the emergence of a spheromak CME configuration at 21 R_Sun, while the solar wind structure in the inner heliosphere is driven by an ADAPT-WSA solution. We demonstrate that even when emerging such a relatively simple CME structure, the simulation reveals strong distortions experienced by a CME due to interactions with slow and fast solar wind streams, in addition to the highly irregular shape of the subsequent CME-driven shock and sheath. This simulation provides insights into the mesoscale structures that form as CMEs dynamically interact with their ambient surroundings at an unprecedented resolution.