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We investigate the impact of bursty star formation on several galaxy scalingrelations of dwarf galaxies using the $\texttt{GRUMPY}$ galaxy formation model.While this model reproduces the star formation rate (SFR)-stellar mass, stellarmass-gas mass, and stellar mass-metallicity relations, the scatter of theserelations in the original model is smaller than observed. We explore theeffects of additional stochasticity of SFR on the scaling relations using amodel that reproduces the level of SFR burstiness in high-resolution zoom-insimulations. The additional SFR stochasticity increases the scatter in theSFR-stellar mass relation to a level similar to that exhibited by most nearbydwarf galaxies. The most extreme observed starbursting dwarfs, however, requirehigher levels of SFR stochasticity. We find that bursty star formationincreases the scatter in the colour-magnitude distribution (CMD) for brighterdwarf galaxies $(M_V < -12)$ to the observed level, but not for fainter onesfor which scatter remains significantly smaller than observed. This is due tothe predominant old stellar populations in these faint model galaxies and theirgenerally declining SFR over the past 10 Gyrs, rather than quenching caused byreionization. We examine the possibility that the colour scatter is due toscatter in metallicity, but show that the level of scatter required leads to anoverestimation of scatter in the metallicity-mass relation. This illustratesthat the scatter of observed scaling relations in the dwarf galaxy regimerepresents a powerful constraint on the properties of their star formation.

Modelling Stochastic Star Formation History of Dwarf Galaxies in GRUMPY