Abstract We present a five-year study of the temporal stability of Jupiter's zonal wind velocity profile at cloud level based on Hubble Space Telescope images obtained from 1995 to 2000. We used the correlation of east–west albedo scans in pairs of images separated by one jovian rotation to retrieve the zonal winds. The resolution in the HST images ranged from 140 to 190 km pixel −1 . Independent measurements of the motions of individual cloud tracers were used to control the above profiles. Three wavelengths were used in this analysis: 410 nm (violet continuum), 892 nm (methane absorption band) and 953 nm (red continuum). Our study indicates that, globally, Jupiter's zonal flow did not change during this five-year interval and it does not depend on the observed wavelengths. When comparing our mean profile with that obtained 16 years ago using Voyager data, we find a reasonable agreement. We note, however, a small shift in the latitude of the jets poleward of latitude ±30°, probably due to image navigation uncertainties. However, true changes in the intensity of the jets at 24°N and 32°N are found. Results also indicate that the 7°S jet has remained stable since the Voyager era. In addition, we extend in this paper our previous study of the 24°N with new data from year 2000. The new data confirm the jet's stability during the 1995–2000 period. Finally we present the average profile for this period, including error estimation, in a table that extends the latitudinal coverage of Limaye's (1986, Icarus 65 , 335–352) Voyager profile up to latitudes ∼68°S and 77°N.