Determining the filaments and their properties in cosmological simulationsIlc, Samo (Avtor) Fabjan, Dunja (Mentor) Galaxies: clusters: generalHydrodynamicsLarge-scale structure of UniverseMethods: numericalIntergalactic mediumCosmological simulations are ideal methods where the evolution of the cosmic web can be studied, allowing for easier insight into the nature of the filaments. We investigate how the intrinsic properties of filaments evolve in areas extracted from a larger cosmological simulation. We selected a subset of regions from the Dianoga simulation to study the filaments and their contents. We analyzed these regions, which were simulated with different baryon physics, namely with and without active galactic nuclei feedback. We constructed the cosmic web using the Sub-space Constrained Mean Shift algorithm and the Sequential Chain Algorithm for Resolving Filaments. We examined the basic physical properties of filaments, including their length, shape, mass, and radius, and analyzed different gas phases (hot, warm-hot intergalactic medium, and colder gas components) within these structures. The evolution of the global filament properties and the properties of the gas phases were studied in the redshift range $0 < z < 1.48$. We confirmed that the shape of the filaments correlates with their length; the longer they are, the more likely they are curved. We find that the scaling relation between the mass $M$ and length $L$ of the filaments is well described by the power law $M\propto L^{1.7}$. The radial density profile widens with redshift, meaning that the radius of the filaments counterintuitively increases over time. The gas mass fraction in the warm-hot intergalactic medium phase does not depend on the physical model and rises towards lower redshifts. However, the included baryon physics significantly impacts the metallicity of gas in filaments since active galactic nuclei feedback affects the metal content already at redshifts of $z\sim 2$. Filament properties are affected by clusters if they lie inside their splashback radius, increasing their mass, gas mass fraction, metallicity and temperature. The more massive the cluster is, the more affected the filament connected to it is.20242024-10-02 08:15:06Doktorsko delo/naloga163090sl