Abstract
Observational studies before and during the flare start were made in Hα (3-λ heliograph at Meudon Observatory) on a large sample of ‘elementary’ flares, both on the disk and along the limb of the Sun. The concept of elementary eruptive phenomenon (EEP) is proposed to describe these observational data. The EEP may be considered as the basic element of complex flares which, then, are built up by the juxtaposition of several EEP. In the inferred scenario, the chromospheric eruptive phenomenon consists of two systems of loops: one cold - the surging arch -T∼- 104 K, the other hot - the flaring arch -, covering a temperature range up to 107 K. The footpoints of the two systems remain differentiated until extinction of the phenomenon; their behaviour over time differs also. The surging arch (the magnetic flux emergence) rises first progressively in the solar atmosphere and the upper part of the loop is heated to coronal temperatures. The classical surge which is observed in the center of the Hα line, after the flash phase of the flare, is only the late development of the surging arch. The flaring arch originates from a pre-existing low loop, which is also able to rise in the solar atmosphere. These two systems coexist and may combine to form such physical characteristics as mass motion, expansion and post-flash phase.
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Mouradian, Z., Martres, M.J. & Soru-Escaut, I. The emerging magnetic flux and the elementary eruptive phenomenon. Sol Phys 87, 309–328 (1983). https://doi.org/10.1007/BF00224843
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DOI: https://doi.org/10.1007/BF00224843