Authors: Nicolas Trueba (CfA), John Raymond (CfA), Cooper Downs (PSI), Chengcai Shen (CfA), Roberto Lionello (PSI), Nick Murphy (CfA), Susan Lepri (Michigan), Katharine Reeves (CfA), Yeimy Rivera (CfA), Maurice Wilson (HAO)

Shock waves are a key component of many CME events, carrying a significant fraction of the total CME energy and are prominent sites for acceleration of solar energetic particles (SEPs). In this study, we present a 3D model of a limb shock wave triggered by a CME on 2010 June 13 observed with SDO/AIA. Our approach combines the observed kinematics and geometry of the shock bubble with pre-shock coronal conditions obtained from an MAS simulation, a global MHD coronal model, in order to calculate shock jump conditions and, ultimately, reproduce AIA observations of the event. The evolving shock front and downstream shocked gas is modeled in 3D, thereby capturing all components of the shock bubble along the line-of-sight. Crucially, we modeled the time-dependent ionization in the rapidly heated shocked gas to more accurately reflect the changing intensity in each AIA channel. This work aims to examine the effects of pre-shock coronal structure, shock front geometry, and magnetic field alignment on the propagating shock front via plasma diagnostics, as well as an observed type II radio burst.