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Three-dimensional, magnetohydrodynamical simulations of the formation and evolution of planetary nebulae are discussed, and we confirm that planetary nebula jets and ansae can be obtained by magnetic collimation of their central, post-asymptotic giant branch, fast winds. Jets and ansae form at the polar regions as a result of the magnetic tension produced by the magnetized winds. Exterior density distributions anisotropic with latitude (e.g., accretion disks, wind-compressed disks, etc.) aredoi:10.1086/316796 fatcat:rd2zpueqyjbzlnjv3gvtlvumem