Authors: Jesse Wilson (Florida Instititute of Technology), Juan Carlos Palacios (Florida Institute of Technology), Jean Perez (Florida Institute of Technology), Sofianne Bourouaine (Florida Institute of Technology)

The fluid nature of the solar wind presents a unique environment for probing fundamental plasma dynamics. Its turbulent nature describes a nonlinear interaction process, transporting energy from large scales consisting of coherent, organized flow to smaller scales until we reach the dissipation range. However, in magnetized plasmas, observations and simulations reveal the presence of strong, sporadic fluctuations in the direction of flow, describing what we now know as intermittency. By employing the use of structure functions and their associated probability distribution functions (PDFs), we observe that a key characteristic of intermittency is the departure from Gaussian statistics at smaller and smaller scales. We utilize the normal inverse Gaussian (NIG) distribution to model the PDFs, and examine the function parameters across radial proximity to the sun. We aim to capture repeated conditions across the trajectory of orbits 5 through 12 from the Solar Orbiter probe (SolO) in order to construct scaling arguments for those function parameters for length scales within the inertial range. By developing a model to describe a possible evolution of the NIG function, we further our understanding of the mechanisms that drive turbulence and energy transport in the solar wind.