Authors: Sagar Ghimire (UAH), Laxman Adhikari (UAH), Gary P. Zank (UAH), Ashutosh Giri (UAH), and Bishwas L. Shrestha (Princeton University)

The solar wind is a magnetized, expanding plasma whose turbulent fluctuations evolve as they propagate away from the Sun. Using Parker Solar Probe observations from Encounters 1–23, this study examines how key plasma and turbulence quantities vary with heliocentric distance according to geometry composed of the mean-magnetic field and mean solar wind speed–represented by theta_BV; fluctuating magnetic field and velcoity–represented by theta_{delta b} {delta v}, and outward and inward waves–indicated by theta_{ z^+ z^-}. The results show that density, magnetic-field, Alfv’en speed, magnetic fluctuation energy, Elsasser energies, and total turbulent energy generally decrease with heliocentric distance, while solar-wind speed and plasma beta tend to increase outward. However, their radial trends are not identical across different angular geometries. In particular, sigma_c and sigma_D are clearly organized according to theta_{{delta v} {delta b}, and theta_{z^{+}z^{-}}, respectively. The turbulent energy and density exhibit positive correlation as a function of theta_{BV} throughout the inner heliosphere.