  Dense stellar winds may mass-load the jets of active galactic nuclei,
although it is unclear what are the time and spatial scales in which the mixing
takes place. We study the first steps of the interaction between jets and
stellar winds, and also the scales at which the stellar wind may mix with the
jet and mass-load it. We present a detailed two-dimensional simulation,
including thermal cooling, of a bubble formed by the wind of a star. We also
study the first interaction of the wind bubble with the jet using a
three-dimensional simulation in which the star enters the jet. Stability
analysis is carried out for the shocked wind structure, to evaluate the
distances over which the jet-dragged wind, which forms a tail, can propagate
without mixing with the jet flow. The two-dimensional simulations point at
quick wind bubble expansion and fragmentation after about one bubble shock
crossing time. Three-dimensional simulations and stability analysis point at
local mixing in the case of strong perturbations and relatively small density
ratios between the jet and the jet dragged-wind, and to a possibly more stable
shocked wind structure at the phase of maximum tail mass flux. Analytical
estimates also indicate that very early stages of the star jet-penetration time
may be also relevant for mass loading. The combination of these and previous
results from the literature suggest highly unstable interaction structures and
efficient wind-jet flow mixing on the scale of the jet interaction height,
possibly producing strong inhomogeneities within the jet. In addition, the
initial wind bubble shocked by the jet leads to a transient, large interaction
surface. The interaction structure can be a source of significant non-thermal
emission.
