  Using the newly developed code \emph{Menura}, we present the first global
picture of the interaction between a turbulent solar wind and a planetary
obstacle in our solar system, namely a comet. This first publication aims at
shedding lights on the macroscopic effect of the upstream solar wind turbulence
on the induced magnetosphere of a comet. Using a hybrid Particle In Cell
simulation code, we model a medium activity comet, using both a turbulent and a
laminar solar wind input, for a direct comparison between the two regimes. We
show how the turbulent characteristics of the solar wind lead to a smaller
obstacle size. We then present how the upstream turbulent structures, traced by
the perpendicular magnetic field fluctuations absent in the laminar case,
self-consistently drape and pile-up around the denser inner coma, forming
intense plasmoids downstream of the nucleus, pulling away dense cometary ion
bubbles. This pseudo-periodic erosion phenomenon re-channels the global
cometary ion escape and as a result, the innermost coma is found to be on
average 45\% less dense in the turbulent case than predicted by simulating a
laminar upstream flow.
