  In the theoretical framework of hierarchical structure formation, galaxy
clusters evolve through continuous accretion and mergers of substructures.
Cosmological simulations have revealed the best picture of the Universe as a
3-D filamentary network of dark-matter distribution called the cosmic web.
Galaxy clusters are found to form at the nodes of this network and are the
regions of high merging activity. Such mergers being highly energetic, contain
a wealth of information about the dynamical evolution of structures in the
Universe. Observational validation of this scenario needs a colossal effort to
identify numerous events from all-sky surveys. Therefore, such efforts are
sparse in literature and tend to focus on individual systems. In this work, we
present an improved search algorithm for identifying interacting galaxy
clusters and have successfully produced a comprehensive list of systems from
SDSS DR-17. By proposing a set of physically motivated criteria, we classified
these interacting clusters into two broad classes, 'merging' and
'pre-merging/postmerging' systems. Interestingly, as predicted by simulations,
we found that most cases show cluster interaction along the prominent cosmic
filaments of galaxy distribution (i.e., the proxy for DM filaments), with the
most violent ones at their nodes. Moreover, we traced the imprint of
interactions through multi-band signatures, such as diffuse cluster emissions
in radio or X-rays. Although we could not find direct evidence of diffuse
emission from connecting filaments and ridges; our catalogue of interacting
clusters will ease locating such faintest emissions as data from sensitive
telescopes like eROSITA or SKA, becomes accessible
