Formation of a Kinked Alignment of Solar Active Region

  • R. Matsumoto
  • T. Tajima
  • W. Chou
  • K. Shibata

Abstract

Images of the solar corona as observed by the soft X-ray telescope aboard the Yohkoh satellite sometimes show a sequence of S-shaped X-ray emitting regions in the low latitudes of the northern or southern hemisphere (Matsumoto et al. 1996). Such a structure suggests that they are emergent portions of a submerged large scale helical flux tube in the convection zone. When the magnetic twist exceeds a threshold value, the flux tube deforms itself into a helical structure through the kink instability. We have carried out three-dimensional MHD simulations of such a kink-unstable flux tube in a convectively unstable gas layer. Here we briefly describe our model and numerical results (see Matsumoto et al. 1996 for details).

Keywords

Solar Corona Flux Tube Convection Zone Solar Active Region Photospheric Magnetic Field 
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.

References

  1. Matsumoto, R., Tajima, T., Chou, W., Okubo, A., and Shibata, K. (1996) to be submitted to Astrophysical Journal Letters Google Scholar

Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • R. Matsumoto
    • 1
    • 2
  • T. Tajima
    • 3
  • W. Chou
    • 3
  • K. Shibata
    • 4
  1. 1.Department of PhysicsChiba UniversityInage-kuJapan
  2. 2.ASRC, JAERINakaJapan
  3. 3.University of Texas at AustinAustinUSA
  4. 4.National Astronomical ObservatoryMitakaJapan

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