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We present three-dimensional numerical simulations of the rise andfragmentation of twisted, initially horizontal magnetic flux tubes which evolveinto emerging Omega-loops. The flux tubes rise buoyantly through anadiabatically stratified plasma that represents the solar convection zone. TheMHD equations are solved in the anelastic approximation, and the results arecompared with studies of flux tube fragmentation in two dimensions. We findthat if the initial amount of field line twist is below a critical value, thedegree of fragmentation at the apex of a rising Omega-loop depends on itsthree-dimensional geometry: the greater the apex curvature of a givenOmega-loop, the lesser the degree of fragmentation of the loop as it approachesthe photosphere. Thus, the amount of initial twist necessary for the loop toretain its cohesion can be reduced substantially from the two-dimensionallimit. The simulations also suggest that as a fragmented flux tube emergesthrough a relatively quiet portion of the solar disk, extended crescent-shapedmagnetic features of opposite polarity should form and steadily recede from oneanother. These features eventually coalesce after the fragmented portion of theOmega-loop emerges through the photosphere.Comment: 17 pages, 17 figures, uses AAS LaTeX macros v5.0. ApJ, in pres

The Three‐dimensional Evolution of Rising, Twisted Magnetic Flux Tubes in a Gravitationally Stratified Model Convection Zone