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Using 3D radiation-hydrodynamical simulations, we study the effects ofionising radiation on the formation of second-generation (SG) stars in GlobularClusters (GCs) with multiple stellar populations. In particular, we focus onmassive ($10^7 \mathrm{M}_{\odot}$) and young (40-Myr old) GCs. We considerstellar winds from asymptotic giant branch (AGB) stars, ram pressure, gasaccretion onto the cluster, and photoionisation feedback of binary stars. Wefind that the stellar luminosity is strong enough to warm and ionise theintracluster medium, but it does not lead to a significant gas expulsion. Thecluster can thus retain the ejecta of AGB stars and the accreted pristine gas.In addition, efficient cooling occurs in the central region of the clusterwithin $50 \mathrm{Myr}$ from the formation of first generation stars, leadingto the formation of SG stars. Our results indicate that the inclusion ofphotoionisation does not suppress SG formation, but rather delays it by about$\sim10 \mathrm{Myr}$. The time delay depends on the density of the pristinegas, so that a denser medium exhibits a shorter delay in star formation.Moreover, photoionisation leads to a modest decrease in the total SG mass,compared to a model without it.

Ionising Feedback Effects on Star Formation in Globular Clusters with Multiple Stellar Populations