NUMERICAL COMPUTATIONS OF NON-LINEAR WAVES IN SOLAR ATMOSPHERE

We computed the upward propagation and evolution of different kinds of perturbations in the solar atmosphere,using HSRA as the unperturbed model.The dynamical equation used is an one dimensional compressible flow equation under gravitational acceleration at the solar surface.Polytropic gas equations of different γ's are used to close this equation set.Our results show that an upward progagated small perturbation can evolve into shocks at certain heights which are nearly independent of the thermodynamic processes involved,but depending strongly upon the strength of the initial perturbation.But the existence and interference of the turbalent field in the solar atmosphere will not allow these perturbations to develop into shocks.This confirms the idea that the mechanical waves generated from the convection zone are not very effective in heating the chromosphere and corona.