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

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

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..970s&link_type=abstract

Astrophysical Journal, Part 1, vol. 263, Dec. 15, 1982, p. 970-981.

Astronomy and Astrophysics

Astrophysics

13

Coronal Loops, Magnetoacoustic Waves, Magnetohydrodynamic Stability, Solar Flares, Solar Prominences, Stellar Models, Coupled Modes, Kinetic Equations, Plasma Heating, Ponderomotive Forces, Solar Magnetic Field, Wave Propagation

Scientific paper

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 γ ≍ k||υAβ1/2(1+I0)1/2 / 2.6 I1/20, when the incident wave intensity I0 exceeds a critical value Ic given by Ic = (ΔBc/B0)2 = 0.3 C2s/υ2g.

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