The INFERNO model

The INFERNO model samples individual stars assuming an initial mass function, then traces these stars as individual particles in the simulation (see Andersson et al., 2020, 2021, 2023). Stellar evolution is tracked for each star, modeling the injection of energy, momentum, and chemically enriched material from stellar winds (fast winds from O & B type stars, as well as post-main-sequence giants), core-collapse supernovae, and type Ia supernovae. Unresolved collisional dynamics are treated by applying natal kicks to simulate walkaway and runaway stars. INFERNO is implemented in the N-body and hydrodynamics code RAMSES (Teyssier, 2002). The model is optimized for galaxy-scale simulations and has been applied in a cosmological environment using the zoom-in technique (Andersson et al., 2024).