Heating of Slow Winds
The 1D hydrodynamic description of turbulence presented in the previous chapter has proven to be useful as a first approach to understand the development of turbulence in the expanding box simulations. However the 3D MHD model introduced in Sect. 2.2, the EBM equations, is clearly more realistic. In this chapter, we detail the initial properties of the plasma selected in our slow wind simulations. Then, we give the methods used to evaluate turbulent heating in our numerical simulations. Finally, we present the numerical results and the conclusions.
- 3.Montagud-Camps V, Grappin R, Verdini A (2018) Turbulent Heating between 0.2 and 1 au: a numerical study. Astrophys J 853(2):153. https://doi.org/10.3847/1538-4357/aaa1ea
- 5.Vasquez BJ, Smith CW, Hamilton K, MacBride BT, Leamon RJ (2007) Evaluation of the turbulent energy cascade rates from the upper inertial range in the solar wind at 1 AU. J Geophys Res 112(A7). https://doi.org/10.1029/2007JA012305