  With a hydrodynamical simulation using a simple galaxy formation model
without taking into account feedback, our previous work has shown that dense
and massive filaments at high redshift can provide potential wells to trap and
compress gas, and hence affect galaxy formation in their resident low-mass
haloes. In this paper, we make use of the Auriga simulations, a suite of
high-resolution zoom-in hydrodynamical simulations of Milky Way-like galaxies,
to study whether the conclusion still holds in the simulations with a
sophisticated galaxy formation model. In agreement with the results of our
previous work, we find that, comparing to their counterparts with similar halo
masses in field, dwarf galaxies residing in filaments tend to have higher
baryonic and stellar fractions. At the fixed parent halo mass, the filament
dwarfs tend to have slightly higher star formation rates than those of field
ones. But overall we do not find a clear difference in galaxy g - r colours
between the filament and field populations. We also show that at high
redshifts, the gas components in dwarf galaxies tend to have their spins
aligned with the filaments in which they reside. Our results support a picture
in which massive filaments at high redshift assist gas accretion and enhance
star formation in their resident dwarf sized dark matter haloes.
