We study MHD wave propagation in a gravitationally stratified isothermal viscous atmosphere of the Sun, permeated by a uniform magentic field. We perform numerical simulations by launching a slow wave on the upper boundary. The driven slow wave propagates down from lowβ- to high-β plasma across the region where the plasma β is unity. It is found that mode conversion takes place at z ≈ -1.8 in the layer β ≈ 1. The amplitudes of horizontal and vertical velocites are smaller than those obtained in the absence of viscosity.

ABSTRACT
1. INTRODUCTION
2. BASIC EQUATIONS AND BOUNDARY CONDI-TIONS
3. NUMERICAL RESULTS AND DISCUSSION
4. CONCLUSIONS
REFERENCES

• Nagendra Kumar(Department of Mathematics, M. M. H. College)
• Anil Kumar(Department of Mathematics, Maharaja Agrasen Institute of Technology)
• K. Murawski(Group of Astrophysics, Institute of Physics)