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The occurrence rate of close-in super-Earths is higher around M-dwarfs compared to stars of higher masses. In this work, we aim to understand how the super-Earth population is affected by the stellar mass, the size of the protoplanetary disc, and viscous heating. We utilised a standard protoplanetary disc model with both irradiated and viscous heating, together with a pebble accretion model, to si
