However, as the heat input to the heavy ions increases, the dependence of these parameters on the abundance goes through a transition and starts to follow the opposite pattern, namely a decrease in flow speed and proton temperature at 1 AU, and an increase in proton mass flux. This study shows that, for currently known photospheric elemental abundances, the flow properties of heavy ions cannot be investigated independently of those of the bulk proton-electron solar wind when the energy transfer between them becomes significant. The effect of heavy ions on the electron-proton bulk solar wind is determined primarily by the collisions occurring very close to the coronal base. Hence, including physical processes responsible for the preferential heating of heavy ions to temperatures exceeding those of protons in the inner corona, cannot be done without considering the subsequent implications for the protons and electrons in a self-consistent manner. The energy from wave damping or turbulence dissipation is assumed to be apportioned to different ions.
Alfven waves tend to decrease the velocity difference between minor ions and protons.
When minor ions surpass the proton speed because of their preferential heating and reach the local Alfven wave phase speed, the minor ions will suffer a drag force from Alfven waves which makes them flow slower. The two observation facts, that heavy ions flow faster than protons, and that they are hotter than protons, are linked by a common explanation. The temperatures of heavy ions at 1AU are reasonable compared to observations. The well-known mass proportional temperatures of heavy ions are found in our models. We show in this Letter how the component of the kinetic temperature in the direction perpendicular to the magnetic field, for both isotropic and anisotropic temperature distributions, affects both the amount of Doppler dimming and pumping.