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Relativistic outflows represent one of the best-suited tools to probe thephysics of AGN. Numerical modelling of internal structure of the relativisticoutflows on parsec scales provides important clues about the conditions anddynamics of the material in the immediate vicinity of the central black holesin AGN. We investigate possible causes of the structural patterns andregularities observed in the parsec-scale jet of the well-known quasar 3C 273.We present here the results from a 3D relativistic hydrodynamics numericalsimulation based on the parameters given for the jet by Lobanov & Zensus(2001), and one in which the effects of jet precession and the injection ofdiscrete components have been taken into account. We compare the model with thestructures observed in 3C 273 using very long baseline interferometry andconstrain the basic properties of the flow. We find growing perturbation modesin the simulation with similar wavelengths to those observed, but with adifferent set of wave speeds and mode identification. If the observed longesthelical structure is produced by the precession of the flow, longer precessionperiods should be expected. Our results show that some of the observedstructures could be explained by growing Kelvin-Helmholtz instabilities in aslow moving region of the jet. However, we point towards possible errors in themode identification that show the need of more complete linear analysis inorder to interpret the observations. We conclude that, with the given viewingangle, superluminal components and jet precession cannot explain the observedstructures.

The role of Kelvin-Helmholtz instability in the internal structure of relativistic outflows. The case of the jet in 3C 273