  Hydrodynamical cosmological simulations are ideal laboratories where the
evolution of the cosmic web can be studied. This allows for easier insight into
the nature of the filaments. We investigate how the intrinsic properties of
filaments are evolving in areas extracted from a larger cosmological
simulation. We aim to identify significant trends in the properties of Warm-Hot
Intergalactic Medium (WHIM) and suggest possible explanations. To study the
filaments and their contents, we select a subset of regions from the Dianoga
simulation. We analysed these regions that were simulated with different baryon
physics, namely with and without the AGN feedback. We construct the cosmic web
using the Sub-space Constrained Mean Shift (SCMS) algorithm and the Sequential
Chain Algorithm for Resolving Filaments (SCARF). We examined the basic physical
properties of filaments (length, shape, mass, radius) and analysed different
gas phases (hot, WHIM and colder gas components) within those structures. The
evolution of the global filament properties and the properties of the gas
phases were studied in the redshift range $0 < z < 1.48$. Within our
simulations, the detected filaments have, on average, lengths below $9$ Mpc.
The filaments' shape correlates with their length; the longer they are, the
more likely they are curved. We find that the scaling relation between mass $M$
and length $L$ of the filaments is well described by the power law $M \propto
L^{1.7}$. The radial density profile is widening with redshift, meaning that
the radius of the filaments is getting larger over time. The fraction of gas
mass in the WHIM phase does not depend on the model and is rising towards lower
redshifts. However, the included baryon physics has a strong impact on the
metallicity of gas in filaments, indicating that the AGN feedback impacts the
metal content already at redshifts of $z \sim 2$.
