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Since its discovery in the aurorae of Jupiter ~30 years ago, the H$_{3}^{+}$ion has served as an invaluable probe of giant planet upper atmospheres.However, the vast majority of monitoring of planetary H$_{3}^{+}$ radiation hasfollowed from observations that rely on deriving parameters fromcolumn-integrated paths through the emitting layer. Here, we investigate theeffects of density and temperature gradients along such paths on the measuredH$_{3}^{+}$ spectrum and its resulting interpretation. In a non-isothermalatmosphere, H$_{3}^{+}$ column densities retrieved from such observations arefound to represent a lower limit, reduced by 20% or more from the trueatmospheric value. Global simulations of Uranus' ionosphere reveal thatmeasured H$_{3}^{+}$ temperature variations are often attributable towell-understood solar zenith angle effects rather than indications of realatmospheric variability. Finally, based on these insights, a preliminary methodof deriving vertical temperature structure is demonstrated at Jupiter usingmodel reproductions of electron density and H$_{3}^{+}$ measurements. The sheerdiversity and uncertainty of conditions in planetary atmospheres prohibits thiswork from providing blanket quantitative correction factors; nonetheless, weillustrate a few simple ways in which the already formidable utility ofH$_{3}^{+}$ observations in understanding planetary atmospheres can beenhanced.

philosophical transactions - royal society. mathematical, physical and engineering sciences/philosophical transactions - royal society. mathematical, physical and engineering sciences

Modelling H$_{3}^{+}$ in planetary atmospheres: effects of vertical gradients on observed quantities