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Protostellar jets and winds are probably driven magnetocentrifugally from thesurface of accretion disks close to the central stellar objects. The exactlaunching conditions on the disk, such as the distributions of magnetic fluxand mass ejection rate, are poorly unknown. They could be constrained fromobservations at large distances, provided that a robust model is available tolink the observable properties of the jets and winds at the large distances tothe conditions at the base of the flow. We discuss the difficulties inconstructing such large-scale wind models, and describe a novel technique whichenables us to numerically follow the acceleration and propagation of the windfrom the disk surface to arbitrarily large distances and the collimation ofpart of the wind into a dense, narrow ``jet'' around the rotation axis. Specialattention is paid to the shape of the jet and its mass flux relative to that ofthe whole wind. The mass flux ratio is a measure of the jet formationefficiency.Comment: 6 pages, figures included. To appear in "The Origins of Stars and  Planets: The VLT View". J. Alves and M. McCaughrean, editor

Structure of Magnetocentrifugal Disk-Winds: From the Launching Surface to Large Distances