Globular clusters, for long considered single stellar populations, recently revealed their real complex nature. Most of them, if not all, show star-to-star variations in the content of light elements, and few massive ones seem to host stellar populations with different metallicities. The origin of such anomalies is currently among the most debated open questions in stellar astrophysics. In this talk I will present a series of N-body models that follow the entire evolution of globular clusters orbiting the Galaxy, while they form their multiple stellar populations, suffer from stellar evolution as well as mutual interactions and mergers, producing systems similar to the observed ones. These models are the framework to interpret and exploit existing and future observational data (e.g. from Gaia, 4MOST, WEAVE, JWST and ELT) to shed light on the origin of the chemical peculiarities in globular clusters.
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