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We present 2D axisymmetric and 3D numerical simulations of theproto-planetary nebula Hen 3-1475, which is characterized by a remarkablyhighly collimated optical jet, formed by a string of shock-excited knots alongthe axis of the nebula. It has recently been suggested that the kinematical andmorphological properties of the Hen 3-1475 jet could be the result of anejection variability of the central source (Riera et al. 2003). Theobservations suggest a periodic variability of the ejection velocitysuperimposed on a smoothly increasing ejection velocity ramp. From ournumerical simulations, we have obtained intensity maps (for different opticalemission lines) and position-velocity diagrams, in order to make a directcomparison with the HST observations of this object. Our numerical study allowsus to conclude that a model of a precessing jet with a time-dependent ejectionvelocity, which is propagating into an ISM previously perturbed by an AGB wind,can succesfully explain both the morphological and the kinematicalcharacteristics of this proto-planetary nebula.Comment: Astronomy and Astrophysics (accepted) (8 figures

Time-dependent ejection velocity model for the outflow of Hen 3-1475