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Using zoom-simulations carried out with the adaptive mesh-refinement codeRAMSES with a dynamic range of up to $2^{27} \approx 1.34 \times 10^8$ weinvestigate the accretion profiles around six stars embedded in differentenvironments inside a (40 pc)$^3$ giant molecular cloud, the role of massinfall and disc instabilities on the accretion profile, and thus on theluminosity of the forming protostar. Our results show that the environment inwhich the protostar is embedded determines the overall accretion profile of theprotostar. Infall on to the circumstellar disc may trigger gravitational discinstabilities in the disc at distances of around ~10 to ~50 au leading to rapidtransport of angular momentum and strong accretion bursts. These burststypically last for about ~10 to a ~100 yr, consistent with typical orbitaltimes at the location of the instability, and enhance the luminosity of theprotostar. Calculations with the stellar evolution code mesa show that theaccretion bursts induce significant changes in the protostellar proper- ties,such as the stellar temperature and radius. We apply the obtained protostellarproperties to produce synthetic observables with RADMC3D and predict thataccretion bursts lead to ob- servable enhancements around 20 to 200 $\mu$m inthe spectral energy distribution of Class 0 type young stellar objects.

Episodic accretion: the interplay of infall and disc instabilities