Search for a self-consistent solar wind model
Résumé
We describe here a solar wind 1-fluid 1D model which is (1) time-dependent (2) includes transition region down to solar surface (3) uses a moderate number of grid points to enable further generalization to 2D/3D. The present model enables to study the response of the transition region and corona to photospheric pressure perturbations, including the solar wind up to ten solar radii. A simple chromosphere model with uniform temperature is used, in two different forms, either taking into account partial ionization or not. We show here how the amplitude of the response and associated viscous heating vary when attempting to decreasing the dynamical viscosity to approach realistic values.