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<rdf:RDF xmlns:rdf="http://www.w3.org/1999/02/22-rdf-syntax-ns#" xmlns:dc="http://purl.org/dc/elements/1.1/"><rdf:Description rdf:about="https://repozitorij.uni-lj.si/IzpisGradiva.php?id=163142"><dc:title>Properties of the diffuse gas component in filaments detected in the Dianoga cosmological simulations</dc:title><dc:creator>Ilc,	Samo	(Avtor)
	</dc:creator><dc:creator>Fabjan,	Dunja	(Avtor)
	</dc:creator><dc:creator>Rasia,	Elena	(Avtor)
	</dc:creator><dc:creator>Borgani,	Stefano	(Avtor)
	</dc:creator><dc:creator>Dolag,	Klaus	(Avtor)
	</dc:creator><dc:subject>galaxies clusters</dc:subject><dc:subject>intergalactic medium</dc:subject><dc:subject>large-scale structure</dc:subject><dc:description>Context. Cosmic filaments are observationally hard to detect. However, hydrodynamical cosmological simulations are ideal laboratories where the evolution of the cosmic web can be studied, and they allow for easier insight into the nature of the filaments. Aims. 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 the warm-hot intergalactic medium (WHIM) and suggest possible explanations.</dc:description><dc:date>2024</dc:date><dc:date>2024-10-02 15:09:13</dc:date><dc:type>Članek v reviji</dc:type><dc:identifier>163142</dc:identifier><dc:language>sl</dc:language></rdf:Description></rdf:RDF>