  Voids possess a very complex internal structure and dynamics. Using $N$-body
simulations we study the hierarchical nature of sub-structures present in the
cosmic web (CW). We use the SpineWeb method which provides a complete
characterization of the CW into its primary constituents: voids, walls,
filaments, and nodes. We aim to characterize the inner compositions of voids by
detecting their internal filamentary structure and explore the impact of this
on the properties of void galaxies. Using a semi-analytical galaxy evolution
model we explore the impact of the CW on several galaxies' properties. We find
the fraction of haloes living in various CW components to be a function of
their mass, with the majority of the haloes of mass below $10^{12}M_{\odot}/h$,
residing in voids and haloes of higher masses distributed mostly in walls.
Similarly, in the Stellar-to-Halo mass relationship, we observe an
environmental dependence for haloes of masses below $10^{12}M_{\odot}/h$,
showing an increased stellar mass fraction for the densest environments.
  The spin is lower for galaxies in the densest environments for the mass range
of $10^{10}-10^{12}M_{\odot}/h$. Finally, we found a strong trend of higher
metallicity fractions for filaments and node galaxies, with respect to the full
sample, in the range of $M_*<10^{10}M_{\odot}/h$.
  Our results show that cosmic voids possess an intricate internal network of
substructures. This in turn makes them a complex environment for galaxy
formation, impacting in an unique way the properties and evolution of the
chosen few galaxies that form inside them.
