  Dwarf galaxies are thought to quench primarily due to environmental processes
most typically occurring in galaxy groups and clusters or around single,
massive galaxies. However, at earlier epochs, ($5 < z < 2$), the collapse of
large scale structure (forming Zel'dovich sheets and subsequently filaments of
the cosmic web) can produce volume-filling accretion shocks which elevate large
swaths of the intergalactic medium (IGM) in these structures to a hot ($T>10^6$
K) phase. We study the impact of such an event on the evolution of central
dwarf galaxies ($5.5 < \log M_* < 8.5$) in the field using a spatially large,
high resolution cosmological zoom simulation which covers the cosmic web
environment between two protoclusters. We find that the shock-heated sheet acts
as an environmental quencher much like clusters and filaments at lower
redshift, creating a population of quenched, central dwarf galaxies. Even
massive dwarfs which do not quench are affected by the shock, with reductions
to their sSFR and gas accretion. This process can potentially explain the
presence of isolated quenched dwarf galaxies, and represents an avenue of
pre-processing, via which quenched satellites of bound systems quench before
infall.
