The escape and precipitation of planetary ions at Mercury under different solar wind conditions have been examined using a global hybrid simulation. The combination of Mercury’s weak intrinsic magnetic field and solar wind conditions at Mercury’s location results in the formation of a relatively small magnetosphere compared to that of Earth. Its magnetosphere is strongly compressed and may disappear when solar wind conditions are extreme. Under these circumstances, the solar wind can directly interact with the thickest part of the exosphere and surface and the escape of planetary ions is expected to be enhanced. By focusing on the dynamic pressure and interplanetary magnetic field dependence, three different solar wind conditions are used in this study. Under the extreme solar wind conditions, planetary protons shows the highest escape rates while planetary sodium ions show the smallest, indicating that the distribution of the sodium ions around the planet is controlled by the size of the magnetosphere. As the Larmor radius of planetary sodium ions is larger than that of planetary protons, they cannot escape and instead precipitate onto the surface during extreme solar wind conditions, when the dayside magnetosphere is well compressed. The precipitation maps of the solar wind protons, planetary protons, and planetary sodium ions) show that the flux from planetary plasmas is sometimes higher than the flux of solar wind plasmas, suggesting that the precipitation of planetary plasmas are probably a non-negligible source of the space weathering of Mercury’s surface, in particular during extreme solar wind conditions.