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We investigate the development of the colour-magnitude re- lation (CMR) ofcluster galaxies. This study is carried out using a semi- analytic model ofgalaxy formation and evolution coupled to a sample of simulated galaxy clustersof different masses, reinforcing the conclusions reached by Jim\'enez et al.(2009). We compare both simulated and obeserved CMRs in differentcolour-magnitude planes, finding a very good agreement in all cases. Thisindicates that model parameters are correctly tuned, giving accurate values ofthe main properties of galaxies for further use in our study. In the presentwork, we perform a statistical analysis of the relative contribution to thestellar mass and metallicity of galaxies along the CMR by the differentprocesses involved in their formation and evolution (i.e. quiescent starformation, disc instability events and galaxy mergers). Our results show that amix of minor and major dry mergers at low redshifts is relevant in theevolution of the most luminous galaxies in the CMR. These processes contributewith low metallicity stars to the remnant galaxies, thus increasing the galaxymasses without significantly altering their colours. These results are foundfor all simulated clusters, supporting the idea of the universality of the CMRin agreement with observational results.

Chemical effects on the development of the colour-magnitude relation of cluster galaxies