  We conduct hydrodynamical cosmological zoom simulations of fourteen voids to
study the ability of haloes to accrete gas at different locations throughout
the voids at z = 0. Measuring the relative velocity of haloes with respect to
their ambient gas, we find that a tenth of the haloes are expected to be unable
to accrete external gas due to its fast flow passed them (so called 'fast flow
haloes'). These are typically located near void walls. We determine that these
haloes have recently crossed the void wall and are still moving away from it.
their motion counter to that of ambient gas falling towards the void wall
results in fast flows that make external gas accretion very challenging, and
often cause partial gas loss via the resultant ram pressures. Using an
analytical approach, we model the impact of such ram pressures on the gas
inside haloes of different masses. A halo's external gas accretion is typically
cut off, with partial stripping of halo gas. For masses below a few times
10$^{9}$ M$_{\odot}$, their halo gas is heavily truncated but not completely
stripped. We identify numerous examples of haloes with a clear jelly-fish like
gas morphology, indicating their surrounding gas is being swept away, cutting
them off from further external accretion. These results highlight how, even in
the relatively low densities of void walls, a fraction of galaxies can interact
with large-scale flows in a manner that has consequences for their gas content
and ability to accrete gas.
