Formation of a Kinked Alignment of Solar Active Region
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).
KeywordsSolar Corona Flux Tube Convection Zone Solar Active Region Photospheric Magnetic Field
- Matsumoto, R., Tajima, T., Chou, W., Okubo, A., and Shibata, K. (1996) to be submitted to Astrophysical Journal Letters Google Scholar