# Three-dimensional simulation of the fast solar wind driven by compressible magnetohydrodynamic turbulence

## TL;DR

This study uses 3D compressible MHD simulations to demonstrate that the fast solar wind is heated and accelerated by turbulence driven by parametric decay instability and Alfven wave reflection, aligning with the wave/turbulence driven scenario.

## Contribution

It provides a self-consistent 3D simulation showing how compressible MHD turbulence, driven by parametric decay instability, accelerates and heats the fast solar wind.

## Key findings

- Turbulence is imbalanced and anisotropic.
- Density fluctuations originate from parametric decay instability.
- Alfven wave reflection triggers turbulence leading to wind acceleration.

## Abstract

Using a three-dimensional compressible magnetohydrodynamic (MHD) simulation, we have reproduced the fast solar wind in a direct and self-consistent manner, based on the wave/turbulence driven scenario. As a natural consequence of Alfvenic perturbations at its base, highly compressional and turbulent fluctuations are generated, leading to heating and acceleration of the solar wind. The analysis of power spectra and structure functions reveals that the turbulence is characterized by its imbalanced (in the sense of outward Alfvenic fluctuations) and anisotropic nature. The density fluctuation originates from the parametric decay instability of outwardly propagating Alfven waves and plays a significant role in the Alfven wave reflection that triggers turbulence. Our conclusion is that the fast solar wind is heated and accelerated by compressible MHD turbulence driven by parametric decay instability and resultant Alfven wave reflection.