In this paper, the analytical and numerical results of the stability a
nalysis of the accretion disk at the inner boundary is presented. Incl
uding the effect of finite conductivity in the disk dynamics, a simple
calculation considering only the radial perturbation has been carried
out. Within local approximation, it is concluded that the disk is sta
ble to Kelvin-Helmholtz and resistive electromagnetic modes whereas th
e magnetosonic mode can destabilise the disk structure.