In this preliminary study, we outline for the first time the effect of non-thermal line broadening processes (turbulence, random waves, convection) on the shape and intensity of the H Ly-&agr; line resonance scattered from the atmosphere of Jupiter and we show how a non-thermal velocity field, confined to the bulge region, in the upper atmosphere of Jupiter, may account for most of the H Ly-&agr; bulge features. Both the shape and the brightness of the Ly-&agr; line from the bulge region as reported by the IUE instrument and the Voyager UV Spectrometer can be recovered assuming resonant scattering with a total atomic hydrogen [H>~4¿1017 cm-2, and a non-thermal component [H>~2¿1015 cm-2 above the thermopause. ¿ American Geophysical Union 1993