Study of the post-flare loops on 29 July 1973. III - Dynamics of H-alpha loops

Physics

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Astronomical Photography, H Alpha Line, Solar Activity Effects, Solar Flares, Doppler Effect, Frequency Shift, Ribbons, Solar Corona, Solar Observatories, Vertical Distribution

Scientific paper

Bright and dark curvilinear structures observed between the two major chromospheric ribbons during the flare of 29 July 1973 on films from the Big Bear Solar Observatory are interpreted as a typical system of coronal loops joining the inner boundaries of the separating flare ribbons. These observations, made through a 0.25 Å Hα filter, only show small segments of the loops having Doppler shifts within approximately ±22 km s-1 relative to the filter passband centered at Hα, Hα - 0.5 Å or Hα + 0.5 Å. However, from our knowledge of the typical behavior of such loop systems observed at the limb in Hα and at 5303 A, it has been possible to reconstruct an approximate model of the probable development of the loops of the 29 July flare as they would have been viewed at the limb relative to the position of a prominence which began to erupt a few minutes before the start of the flare. It is seen that the loops ascended through the space previously occupied by the filament. On the assumption that Hα fine structures parallel the magnetic field, we can conclude that a dramatic reorientation of the direction of the magnetic field in the corona occurred early in the flare, subsequent to the start of the eruption of the filament and prior to the time that the Hα loops ascended through the space previously occupied by the filament.

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