Solar wind charge exchange (SWCX) generated soft X-rays are used extensively to study the interfaces between charged and neutral particles throughout the solar system. This paper outlines the development of a model of Jupiter’s magnetosheath using MHD derived boundary equations and a combination of in situ Juno measurements and numerical models for neutral and charged particle distributions. These are then used to model SWCX emissions in the Jovian magnetosheath for the O$_{VII}$ triplet to determine if the magnetosheath could be imaged in a similar fashion to the planned SMILE mission at Earth. We determine that whole detector counts per minute range from 10$^{-5\pm1}$ to 10$^{-3\pm1}$ for various spacecraft, and, as such, argue that with current instrument sensitivity it is infeasible to study the X-ray emissions from the Jovian magnetosheath. However, with a theoretical x-ray imager with an effective area of 1m$^2$ and FOV of $120^{\circ}\times120^{\circ}$ increases to a peak of $\sim$10$^{0\pm1}$ c/min when observing from a distance of 40 R$_J$. We also discuss the implications of the low emission rates on other higher signal X-ray observations at Jupiter and the possibility of Saturn being a better target for such a mission.