This thesis benchmarked a new probe of atmospheric dynamics in exoplanet atmospheres by resolving the spectral lines stemming from these far atmospheres and then modelling their line shape taking into account the broadening from atmospheric winds. This gives us a window into atmospheric winds for these far away worlds only limited by the depths of the resolved lines. I resolved the sodium doublet for a wide array of exoplanets and applied the novel modelling technique to the hot Jupiter HD189733b and the ultra hot Jupiter WASP-76b. I found that both are dominated by zonal winds in the lower, and vertical winds in the intermediate atmosphere, a first to date. This novel approach pushes the limits of high-resolution transit spectroscopy, which is evolving from an element detection technique to a more holistic atmospheric characterisation technique.