Authors: Malik H. Walker (JHU), Robert C. Allen (SwRI), George C. Ho (SwRI), Glenn M. Mason (JHU/APL), Christina M.S. Cohen (Caltech), Christina Lee (SSL) ,Christian Möstl (GeoSphere Austria), Emma E. Davies (GeoSphere Austria), Eva Weiler(GeoSphere Austria/University of Graz), Junxiang Hu (NASA GSFC/UAH)

Interplanetary Coronal Mass Ejections (ICMEs) are a key contributor to the energetic particle population within the heliosphere. Though as they propagate outwards from the Sun, interactions with other solar wind structures and general changes to ICME properties can alter particle acceleration efficiency and transport effects at their associated shocks. Currently, this 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, and STEREO-A. Using the magnetic field, plasma, and ion compositional data provided by these spacecraft, we derive both local shock and ion spectral shape parameters. By comparing the changes in these parameters at different stages of ICME propagation, we analyze the connection between the evolution of the local shock conditions and the spectral shape.  To better understand the extent to which the shock associated particle distribution is dependent on radial distance, the conclusions from this work are also discussed in the context of an ongoing theoretical study.