Hydrodynamic simulation of surge prominence
Abstract
The generation of a surge prominence is simulated in terms of a onedimensional hydrodynamic model with a velocity pulse in the upper chromosphere. Equations for the changes of the density, velocity and pressure of a compressible medium with time are solved numerically by the use of the Lax difference scheme on an Euler network for the hydrodynamic effects neglecting diffusion terms due to thermal conductivity and viscosity. In the case of a 5min velocity pulse corresponding to the duration of a weak flare, it is shown that a radial flux develops with a slight rise in temperature and density and a shock wave in the leading side. In the region behind the shock, density is found to increase and a more compact nucleus to be formed representing the surge. The trajectory on the 2% density level is also shown to be in better agreement with experimental data than that calculated based on a pressure pulse of the same duration.
 Publication:

Bolgarska Akademiia Nauk Doklady
 Pub Date:
 1981
 Bibcode:
 1981BlDok..34..915D
 Keywords:

 Chromosphere;
 Hydrodynamic Equations;
 Solar Prominences;
 Solar Simulation;
 Cartesian Coordinates;
 Compressible Fluids;
 Computational Fluid Dynamics;
 Dynamic Models;
 Flow Velocity;
 One Dimensional Flow;
 Plasma Density;
 Solar Flares;
 Solar Limb;
 Stellar Evolution;
 Surges;
 Time Dependence;
 Solar Physics