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Comet Shoemaker-Levy 9 impacted Jupiter in July 1994, leaving itsstratosphere with several new species, among them water vapor (H2O). With theaid of a photochemical model H2O can be used as a dynamical tracer in thejovian stratosphere. In this paper, we aim at constraining vertical eddydiffusion (Kzz) at the levels where H2O resides. We monitored the H2Odisk-averaged emission at 556.936 GHz with the Odin space telescope between2002 and 2019, covering nearly two decades. We analyzed the data with acombination of 1D photochemical and radiative transfer models to constrainvertical eddy diffusion in the stratosphere of Jupiter. The Odin observationsshow us that the emission of H2O has an almost linear decrease of about 40%between 2002 and 2019.We can only reproduce our time series if we increase themagnitude of Kzz in the pressure range where H2O diffuses downward from 2002 to2019, i.e. from ~0.2 mbar to ~5 mbar. However, this modified Kzz isincompatible with hydrocarbon observations. We find that, even if allowance ismade for the initially large abundances of H2O and CO at the impact latitudes,the photochemical conversion of H2O to CO2 is not sufficient to explain theprogressive decline of the H2O line emission, suggestive of additional lossmechanisms. The Kzz we derived from the Odin observations of H2O can only beviewed as an upper limit in the ~0.2 mbar to ~5 mbar pressure range. Theincompatibility between the interpretations made from H2O and hydrocarbonobservations probably results from 1D modeling limitations. Meridionalvariability of H2O, most probably at auroral latitudes, would need to beassessed and compared with that of hydrocarbons to quantify the role of auroralchemistry in the temporal evolution of the H2O abundance since the SL9 impacts.Modeling the temporal evolution of SL9 species with a 2D model would be thenext natural step.

18-year long monitoring of the evolution of H2O vapor in the stratosphere of Jupiter with the Odin space telescope