  From deep imaging data obtained with the Large Binocular Telescope as part of
the Smallest Scale of Hierarchy Survey (SSH), we have discovered low-surface
brightness tidal features around NGC 5238 and UGC 8760, two nearby and
relatively isolated dwarf galaxies with stellar masses of approximately $10^8
M_\odot$ and $2\times10^7 M_\odot$, respectively. In this study, we present
detailed hydrodynamical $N$-body simulations that explain the observed faint
substructures as the outcome of interactions between the dwarf galaxies and
smaller satellite systems. We show that the asymmetric stellar distribution of
NGC 5238 and the low-luminosity substructures observed to the northeast of UGC
8760 can be well attributed to recent interactions with smaller galaxies, each
with a stellar mass roughly a few $10^5 M_\odot$, 50 times less massive than
their respective hosts. In the simulations, these satellites have stellar and
dark-matter masses consistent with the ones predicted by $\Lambda$CDM cosmology
and share properties similar to those of local dwarf galaxies with similar
stellar masses. The satellite-to-main galaxy mass ratio is approximately 1:10
in both cases. This satellite population aligns closely with predictions from
cosmological simulations in terms of the number and mass relative to the host
galaxy mass.
