Flare mechanisms

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Jun 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977mmsai..48..321c&link_type=abstract

Società Astronomica Italiana, Memorie, vol. 48, June 1977, p. 321-331. In Italian.

Physics

Solar Flares, Solar Physics, Stellar Models, Energy Transfer, Evolution (Development), Gravitational Effects, Magnetic Effects, Magnetic Field Configurations, Magnetohydrodynamic Stability, Morphology, Thermal Energy

Scientific paper

The paper considers a 'standard' model of a solar flare as defined by morphology, energetics (thermal, gravitational and magnetic), and temporal evolution; the quantitative data considered are characteristic of a large flare (3 plus magnitude). Detailed consideration is given to the three stages of flare evolution: preparatory, peak, and decay. Flare evolution is discussed in reference to three determining factors: (1) the macroscopic instability which leads to intensification of local currents, (2) plasma turbulence, and (3) particle acceleration mechanisms.

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