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We examine star formation and chemical enrichment in protoclusters (PCs)using cosmological zoom-in hydrodynamic simulations. We find that the totalstar formation rate (SFR) in all PC ($>10^{14.4}\,h^{-1}$M$_\odot$) reaches$>10^4\,\mathrm{M}_\odot \mathrm{yr}^{-1}$ at $z=3$, equivalent to the observedPCs. The SFR in the Core region accounts for about $30\%$ of the total starformation in the PC at $z\gtrsim1$, suggesting the importance of the outerregions to reveal the evolution of galaxy clusters. We find that the total SFRof PC is dominated by galaxies with$10^{10}\,\le\,(\mathrm{M}_\star/M_\odot)\,\le\,10^{11}$, while more massivegalaxies dominate the SFR in the Core. For the chemical abundance evolution, wefind that the higher-density region has a higher metallicity and fasterevolution. We show that the [O/Fe] vs. [Fe/H] relation turns down in the Coreat $z=3.4$ due to the enrichment of Fe by Type Ia supernovae. We find noenvironmental effects for the mass--metallicity relations (MZR) or $\log$(N/O)vs. $12+\log$(O/H) for galaxies. We find that the chemical enrichment in galaxyclusters proceeds faster in the high redshift Universe ($z>1$). Our work willbenefit future tomographic observations, particularly using PCs as uniqueprobes of accelerated structure formation and evolution in high-density regionsof the universe.

Star Formation and Chemical Enrichment in Protoclusters