Energetic particles near the Sun are scattered by solar wind turbulence—random fluctuations in magnetic and electric fields. These particles include solar energetic particles from flares and coronal mass ejections, as well as cosmic rays originating beyond the Solar System. When they reach near-Earth space, they can disrupt satellites, power grids, astronauts, and aircraft systems. This project leverages new data from NASA’s Parker Solar Probe (PSP), which are exploring regions closer to the Sun than any prior missions. The spacecraft measure the solar wind’s magnetic and electric fields, offering an unprecedented view of how turbulence
evolves between the Sun and Earth.

We combine these observations with advanced theories—Second-Order Quasi-Linear Theory (SOQLT) and Unified Non-Linear Transport (UNLT)—to model how energetic particles diffuse both along and across magnetic field lines. This diffusion governs how particles spread through the heliosphere. Improving our understanding of this process will enhance space weather forecasting and support strategies to protect astronauts, satellites, and infrastructure. These insights are especially critical for future long-duration missions to the Moon or Mars, where accurate models of radiation exposure in the near-Sun environment will inform spacecraft and habitat design.