Authors: Anshika Singh (NJIT), Bin Chen (NJIT), Xiaocan Li (Los Alamos National Laboratory), Joel Dahlin (NASA GSFC)

Coronal mass ejections (CMEs) are believed to be driven by the eruption of twisted magnetic flux ropes. The flux ropes may host cool filament, hot coronal plasma, and accelerated particles, exhibiting a variety of thermal and nonthermal emission signatures across different wavelengths. While synthetic white light (WL) and extreme ultraviolet (EUV) signatures of erupting flux ropes have been readily produced, generating synthetic nonthermal emission from CME models has been elusive, requiring particle distributions throughout the eruption. In this study, by combining magnetohydrodynamic simulations of a breakout CME with particle modeling, we aim to produce synthetic emission maps across radio, EUV, and WL wavelengths. The results will help us gain new insights into particle acceleration and transport processes during CME initiation. Here we present synthetic EUV and WL maps during the CME evolution. These observables characterize the thermal plasma, show how the eruption would appear to SDO/AIA and LASCO, and identify the flux rope volume that may host the nonthermal electrons. We also introduce next steps to produce synthetic radio gyrosynchrotron radiation from non-thermal electrons entrained in the CME.