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Despite swift progress in the characterisation of exoplanet atmospheres incomposition and structure, the study of atmospheric dynamics has not progressedat the same speed. While theoretical models have been developed to describe thelower layers of the atmosphere and, disconnected, the exosphere, little isknown about the intermediate layers up to the thermosphere.  We aim to provide a clearer picture of atmospheric dynamics for the class ofultra hot Jupiters, highly-irradiated gas giants, on the example of WASP-76~b.  We analysed two datasets jointly, obtained with the HARPS and ESPRESSOspectrographs, to interpret the resolved planetary sodium doublet. We thenapplied an updated version of the MERC code, with added planetary rotation,also provides the possibility to model the latitude dependence of the windpatterns.  We retrieve the highest Bayesian evidence for an isothermal atmosphere,interpreted as a mean temperature of $3389\pm227$ K, a uniform day-to-nightside wind of $5.5^{+1.4}_{-2.0}\,$ km/s in the lower atmosphere with a verticalwind in the upper atmosphere of $22.7^{+4.9}_{-4.1}\,$ km/s, switchingatmospheric wind patterns at $10^{-3}$ bar above the reference surface pressure($10$ bar).  Our results for WASP-76~b are compatible with previous studies of the loweratmospheric dynamics of WASP-76~b and other ultra hot Jupiters. They highlightthe need for vertical winds in the intermediate atmosphere above the layersprobed by global circulation model studies to explain the line broadening ofthe sodium doublet in this planet. This work demonstrates the capability ofexploiting the resolved spectral line shapes to observationally constrainpossible wind patterns in exoplanet atmospheres, an invaluable input to moresophisticated 3D atmospheric models in the future.

Into the Storm: Diving into the winds of the ultra hot Jupiter WASP-76 b with HARPS and ESPRESSO