Authors: Parisa Mostafavi (JHU/APL), Juan C. P. Palacios (FIT), Vamsee Jagarlamudi (JHU/APL), Sofiane Bourouaine (FIT), Robert Allen (SWRI), George Ho (SWRI), Nour Raouafi (JHU/APL)

Previous observations revealed that solar wind ions exhibit distinct kinetic non-thermal features such as the preferential heating and acceleration of alpha particles compared to protons (the predominant component of the solar wind). Different ion heating mechanisms have been proposed to explain this preferential heating of the alpha particles, although the extent to which these various processes contribute is still not clear. One of the key components in the various ion heating mechanisms is the energy of the turbulent fluctuations near the ion scales. Additionally, local Coulomb collisions and collisional age are indeed important in thermalizing the solar wind plasma populations and reducing the ion non-thermal features. Our goal is to understand how Coulomb collisions and solar wind turbulence affect the heating and acceleration of plasma populations in the inner heliosphere. We analyze observations from Parker Solar Probe and Solar Orbiter to study the collisional effect and turbulence fluctuations at different distances from the Sun.