Flares and velocity fields in AR 5528, AR 5629, and AR 6891

Details Flares and velocity fields in AR 5528, AR 5629, and AR 6891 Flares and velocity fields in AR 5528, AR 5629, and AR 6891

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..150..179c&link_type=abstract

Solar Physics, vol. 150, no. 1-2, p. 179-197

Physics

3

Chromosphere, Line Spectra, Magnetic Field Configurations, Magnetic Field Reconnection, Magnetohydrodynamic Flow, Mathematical Models, Photosphere, Solar Flares, Solar Magnetic Field, Spectral Emission, Sunspots, Velocity Distribution, Vortices, Doppler Effect, Filtergrams, H Beta Line, Images, Kelvin-Helmholtz Instability, Magnetic Signatures, Penumbras, Red Shift, Tearing Modes (Plasmas)

Scientific paper

By analysing the relationship between flares and the morphology of velocity and magnetic fields in active regions AR 5528, AR 5629, and AR 6891, we found that initial brightening points at the earliest phase and flare ribbons at the maximum phase are more closely related to the velocity field patterns than to magnetic field patterns. We also found that the velocity patterns related to the flares are different from Evershed flows in the chromosphere. Finally, a model of vortex-induced reconnection has been applied to solar flares and some preliminary results are discussed.

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