Ballooning instability driven by fast magnetosonic waves and its application to coronal loop transients associated with a flare

A theoretical model for the triggering of coronal loop transients associated with a flare or eruptive prominence is presented. It is suggested that coronal loop transients are due to a ballooning instability in a coronal current loop, which can be driven by fast magnetosonic waves originating from a solar flare: or eruptive prominence: induced disturbance. The coupling equations describing the interaction between ballooning modes and fast magnetosonic waves are derived. It is shown that the ballooning instability driven by fast magnetosonic waves can be excited with the growth rate γroughly-equalk/sub parallel/v/sub A/ β/sup 1/2/(1+I0)/sup 1/2//2.6 I/sup 1/2/0, when the incident wave intensity I0 exceeds a critical value I/sub c/ given by I/sub c/ = (ΔB/sub c//B0)2 = 0.3 C2/sub s//v2/sub g/