出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：We have developed numerical models in order to understand properties of clusters of galaxies,
especially the metal enrichment of the intra-cluster gas (Domainko et al. 2004, [3]). Here we
present the numerical treatment of the dark matter component (DM) and the galaxy formation
process in these combined N-body and hydrodynamic simulations. We study galaxy formation
by identifying dark matter haloes and assigning a galaxy to them in a semi-numerical way. Variations
of different model parameters, like feedback or parameters related to the strength of star
bursts, change the distribution of the baryonic matter in the dark matter halo, influencing galaxy
properties and therefore also the enrichment of the intra-cluster medium (ICM).
Clusters of galaxies consist of many complex physical objects, which are all interacting with each
other, so numerical simulations are probably the best route to a better theoretical understanding.
One unresolved issue is the origin of the heavy elements in the ICM. Neither the efficiency nor the
time dependences of any proposed enrichment process, such as ram-pressure stripping or galactic
winds, are known in detail. We aim at investigating this problem using our simulation method.
