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The star formation history (SFH) of galaxies is critical for understandinggalaxy evolution. Hydrodynamical simulations enable us to precisely reconstructthe SFH of galaxies and establish a link to the underlying physical processes.In this work, we present a model to describe individual galaxies' SFHs fromthree simulations: TheThreeHundred, Illustris-1 and TNG100-1. This modeldivides the galaxy SFH into two distinct components: the "main sequence" andthe "variation". The "main sequence" part is generated by tracing the historyof the $SFR-M_*$ main sequence of galaxies across time. The "variation" partconsists of the scatter around the main sequence, which is reproduced byfractional Brownian motions. We find that: 1) The evolution of the mainsequence varies between simulations; 2) fractional Brownian motions canreproduce many features of SFHs, however, discrepancies still exist; 3) Thevariations and mass-loss rate are crucial for reconstructing the SFHs of thesimulations. This model provides a fair description of the SFHs in simulations.On the other hand, by correlating the fractional Brownian motion model tosimulation data, we provide a 'standard' against which to compare simulations.

A stochastic model to reproduce the star-formation history of individual galaxies in hydrodynamic simulations