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About the Flare Problem

  • K. O. Kiepenheuer
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 2)

Abstract

The macroscopic and microscopic structures of flares are discussed, their relations to spots, to the photospheric magnetic fields and especially to the filaments (prominences) are reviewed. Flares are macroscopically located in a horizontal magnetic field, mostly occupying the dividing line of polarities or the line of vanishing longitudinal field. Flares often reach into regions of very small fields.

Arguments are presented, which make it unprobable that the flare energy is supplied from outside the Hoc-volume. It seems furthermore improbable that the flare phenomenon is a macroscopic explosion or collapse. There is spectroscopic and other evidence for the existence of subtelescopic structures. The close relation between flares and filaments-both show a similar magnetic configuration-lets us suspect that the preflare activation of a filament and the resulting subtelescopic distortions and twistings of the associated magnetic field are the basic processes leading to a flare.

Keywords

Blast Wave Magnetic Configuration Longitudinal Field Photospheric Magnetic Field Magnetic Field Configuration 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Science+Business Media Dordrecht 1965

Authors and Affiliations

  • K. O. Kiepenheuer
    • 1
  1. 1.Fraunhofer InstitutFreiburg i. Br.Germany

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