We report the results of a three-dimensional MHD simulation of the dynamic emergence of a twisted, Ω-shaped tube from the top layer of the solar convection zone into the atmosphere and the corona. It is found that the tube segment at the apex of the Ω-tube expands into the stably stratified atmosphere as a result of the magnetic buoyancy instability (or the Parker instability). Our simulation of the emergence of a left-hand-twisted Ω-tube reproduces several major observed features of a newly developing active region described by Strous and coworkers, including the orientation of the arch-filament system, the distribution of the vertical magnetic field on the photosphere, the locations of sunspot formation, and the organized shear flow pattern in the photospheric horizontal velocity field.
CITATION STYLE
Fan, Y. (2001). The Emergence of a Twisted Ω-Tube into the Solar Atmosphere. The Astrophysical Journal, 554(1), L111–L114. https://doi.org/10.1086/320935
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