About the Flare Problem

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


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.


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.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Athay, R. G. and Moreton, G. E.: 1961, Astrophys. J. 133, 935.ADSCrossRefGoogle Scholar
  2. Becker, U.: 1958, Z. Astrophys. 44, 243.ADSGoogle Scholar
  3. Becker, U.: 1959, Z. Astrophys. 48, 189.ADSGoogle Scholar
  4. Bruzek, A.: 1957, Z. Astrophys. 42, 76.ADSGoogle Scholar
  5. Bruzek, A.: 1958, Z. Astrophys. 44, 183.ADSGoogle Scholar
  6. Bumba, V.: 1958, Izv. Krimsk. Astrofiz. Obs. 19, 105.Google Scholar
  7. Bumba, V.: 1962, Izv. Krimsk. Astrofiz. Obs. 23, 437.Google Scholar
  8. Dodson, Helen W. and Hedeman, E.: 1949, Astrophys. J. 110, 242.ADSCrossRefGoogle Scholar
  9. Fokker, A. D.: 1963, Space Sci. Revs. 2, 88.CrossRefGoogle Scholar
  10. Fortini, T.: 1963, Astrophys. J. 138, 278.ADSCrossRefGoogle Scholar
  11. Gold, T. and Hoyle, F.: 1960, Mon. Not. Roy. Astron. Soc. 120, 89.ADSGoogle Scholar
  12. Hansen, R. and Gordon, D.: 1960, PASP. 72, 194.ADSCrossRefGoogle Scholar
  13. Howard, R. and Severny, A.: 1963, Astrophys. J. 137, 1242.ADSCrossRefGoogle Scholar
  14. Howard, R. and Babcock, H. W.: 1960, Astrophys. J. 132, 218.ADSCrossRefGoogle Scholar
  15. Jefferies, J. T. and Orrall, F. O.: 1961, Astrophys. J. 133, 963.ADSCrossRefGoogle Scholar
  16. Kippenhahn, R. and Schlüter, A.: 1957, Z. Astrophys. 43, 36.ADSzbMATHGoogle Scholar
  17. Martres-Tropéz, M. J. and Pick-Gutman, 1962, Compt. Rend. 254, 3975.Google Scholar
  18. Moreton, G. and Malville, J. M.: 1963, PASP 443, 176.ADSGoogle Scholar
  19. Parker, E. N.: 1963, Astrophys. J. Suppl. 7, 177.ADSCrossRefGoogle Scholar
  20. Smith, S. F. and Ramsey, E.: 1964, Z. Astrophys., 60, 1.ADSGoogle Scholar
  21. Suemoto, Z. and Hiei, E.: 1959, Publ. Astron. Soc. Japan 185, 11.Google Scholar
  22. Sweet, P. A.: 1956, IAU Symposium 6, paper 14.Google Scholar
  23. Unsöld, A.: 1962, Physik der Sternenatmosphären, p. 323.Google Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1965

Authors and Affiliations

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

Personalised recommendations