Authors: J. Grant Mitchell (NASA/GSFC), E. R. Christian (NASA/GSFC), G. A. de Nolfo (NASA/GSFC), C. M. S. Cohen (Caltech), M. E. Hill (JHU/APL), A. Kouloumvakos (JHU/APL), A. W. Labrador (Caltech), R. A. Leske (Caltech), D. J. McComas (Princeton), R. L. McNutt Jr. (JHU/APL), D. G. Mitchell (JHU/APL), M. Shen (Princeton), N. A. Schwadron (UNH), M. E. Wiedenbeck (JPL), S. D. Bale (UC Berkeley), M. Pulupa (UC Berkeley)

For over two decades, it has been observed that near-relativistic electrons appear delayed with respect to electromagnetic emission produced by lower energy electrons, including type III radio bursts.  This has led to a long-standing debate over whether these delays are due to a delayed acceleration of the higher energy electrons or due to delays in transport through the heliosphere.  Parker Solar Probe offers the unique opportunity to investigate these delays at a variety of heliocentric distances.  Our recent study of near-relativistic electron events with the ISOIS instruments on Parker Solar Probe demonstrated a relationship between the delays of near-relativistic electrons with respect to type III radio bursts and the observing distance of the spacecraft (Mitchell et al. 2025).  This discovery led to the conclusion that transport must play a role in the observed delay of near-relativistic electrons. In the present work, we further investigate our growing number of electron events observed close to the Sun as well as the source of the delays observed farther from the Sun through examination of the plasma and electromagnetic conditions through which the electrons propagated with a goal of identifying the primary driver in the delays of these electrons.