Abstract

Mechanisms for the coronal heating and the acceleration of the solar wind are still largely debated. The thorough study of the solar wind for the past 60 years has, however, motivated an important focus on Alfvén waves and turbulence. In this talk, I will review and discuss models for Alfvén wave propagation and turbulent cascade, which eventually leads to dissipation. I will show how turbulent transport models can explain the large scale properties of the solar wind measured by the Parker Solar Probe and Solar Orbiter. In the light of a recent study, we will see why a compressible process the parametric decay instability is essential to the generation of a turbulent power spectrum from a narrow band emission of Alfvén waves at the solar surface. Finally, I will discuss the relation between wave and turbulence and the composition of solar and stellar atmosphere through the first ionization potential  (FIP) and inverse FIP effect.