  We study the properties of associations of dwarf galaxies and their
dependence on the environment. Associations of dwarf galaxies are extended
systems composed exclusively of dwarf galaxies, considering as dwarf galaxies
those galaxies less massive than $M_{\star, \rm max} = 10^{9.0}$ ${\rm
M}_{\odot}\,h^{-1}$. We identify these particular systems using a
semi-analytical model of galaxy formation coupled to a dark matter only
simulation in the $\Lambda$ Cold Dark Matter cosmological model. To classify
the environment, we estimate eigenvalues from the tidal field of the dark
matter particle distribution of the simulation. We find that the majority, two
thirds, of associations are located in filaments ($ \sim 67$ per cent),
followed by walls ($ \sim 26 $ per cent), while only a small fraction of them
are in knots ($ \sim 6 $ per cent) and voids ($ \sim 1 $ per cent).
Associations located in more dense environments present significantly higher
velocity dispersion than those located in less dense environments, evidencing
that the environment plays a fundamental role in their dynamical properties.
However, this connection between velocity dispersion and the environment
depends exclusively on whether the systems are gravitational bound or unbound,
given that it disappears when we consider associations of dwarf galaxies that
are gravitationally bound. Although less than a dozen observationally detected
associations of dwarf galaxies are currently known, our results are predictions
on the eve of forthcoming large surveys of galaxies, which will enable these
very particular systems to be identified and studied.
