Authors: Malik H. Walker (JHU), Robert C. Allen (SwRI), George C. Ho (SwRI), Glenn M. Mason (JHU/APL), Gang Li (General Linear Space Plasma Lab LLC), Christina M.S. Cohen (Caltech), Christina Lee (SSL)

Particles accelerated at the shocks formed by Interplanetary Coronal Mass Ejections (ICMEs) are a key part of the energetic particle population within the heliosphere. While the underlying mechanisms for this process have been studied, the connection between the radial evolution of the ICME-associated shock during propagation and resulting gradual Solar Energetic Particle (SEP) and Energetic Storm Particle (ESP) intensities, composition, and acceleration has yet to be fully uncovered. The recent distributed array of spacecraft at varying distances from the Sun provides a welcome opportunity for an improved statistical analysis of the radial dependency of particle populations and acceleration mechanisms present at ICME-driven shocks. We present the results of a statistical study conducted using our compiled database of multipoint ICME events from 2016-2023, which are observed in situ by Parker Solar Probe (PSP), Solar Orbiter, ACE, Wind, STEREO-A, and MAVEN. From the magnetic field, plasma, and ion composition data provided by these spacecraft, we derive both the observed shock and ion spectral shape parameters. Through the comparison of said parameters for each event, we analyze the radial effects of shock evolution on particle acceleration, allowing for the determination of better constraints on this dependency.