Authors: Manuel Enrique Cuesta (Princeton University), R. Bandyopadhyay (Princeton University), F. Fraschetti (Harvard CFA & Lunar and Planetary Lab), D. J. McComas (Princeton University), C. M. S. Cohen (California Institute of Technology), S. D. Bale (University of California), R. Livi (University of California)

There is an abundance of studies that investigate the spatial diffusion coefficient (\kappa) via simulations and in-situ solar wind observations. However, the relation between \kappa upstream of a shock and the peak intensity of energetic particles at the shock (J_peak) has not been directly investigated to our knowledge. The upstream magnetic fluctuation amplitude (\delta B/B0) is connected to \kappa such that a large \delta B/B0 would reduce \kappa, suggesting that particles are accelerated and trapped for a longer time by the shock. This should result in a larger J_peak. On the contrary, a smaller \delta B/B0 would enhance \kappa such that the acceleration time is shortened, or energetic particles are trapped for a shorter time, resulting in a smaller J_peak. We examine this expected relationship between \kappa, \delta B/B0, and J_peak for several interplanetary shocks observed by Parker Solar Probe. In particular, we use \kappa as a fit parameter of the upstream intensity profile of energetic particles using the diffusive shock acceleration model. The results presented here will help improve the modeling of interplanetary shocks and their production of energetic particles.