Abstract
In the present chapter, we describe the recent results obtained in the development of solar wind models using the kinetic approach. We show how the solution of the evolution equation is used to determine the velocity distribution function (VDF) of the solar wind particles and their moments. The solutions depend on the approximations and assumptions made in the development of the models. We describe in particular the results obtained with the collisionless exospheric approximation, the effects of Coulomb collisions obtained by using a Fokker-Planck term in the evolution equation, the effects of wave turbulence for the electrons and those of kinetic Alfven waves for the protons.
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