Activation of solar flares

P. J. Cargill, S. Migliuolo, A. W. Hood

Research output: Contribution to journalArticlepeer-review


The physics of the activation of two-ribbon solar flares via the MHD instability of coronal arcades is presented. The destabilization of a preflare magnetic field is necessary in order for a rapid energy release, characteristic of the impulsive phase of the flare, to occur. The authors examine the stability of a number of configurations and discuss the physical consequences and relative importance of varying pressure profiles and different sets of boundary conditions (involving field-line tying). Interchange modes, driven unstable by pressure gradients, are candidates for instability. Shearless vs. sheared equilibria are also discussed.
Original languageEnglish
JournalIn ESA Plasma Astrophys. p 57-63 (SEE N85-22270 12-90)
Publication statusPublished - 1 Nov 1984


  • Magnetohydrodynamic Stability
  • Solar Corona
  • Solar Flares
  • Solar Magnetic Field
  • Magnetohydrodynamic Shear Heating
  • Plasma Equilibrium
  • Pressure Gradients
  • Solar Activity Effects


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