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We study how star formation is regulated in low-mass field dwarf galaxies($10^5 \leq M_{\star} \leq 10^6 \, \text{M}_{\odot}$), using cosmologicalhigh-resolution ($3 \, \text{pc}$) hydrodynamical simulations. Cosmicreionization quenches star formation in all our simulated dwarfs, but threegalaxies with final dynamical masses of $3 \times 10^{9} \,\text{M}_{\odot}$are subsequently able to replenish their interstellar medium by slowlyaccreting gas. Two of these galaxies re-ignite and sustain star formation untilthe present day at an average rate of $10^{-5} \, \text{M}_{\odot} \,\text{yr}^{-1}$, highly reminiscent of observed low-mass star-forming dwarfirregulars such as Leo T. The resumption of star formation is delayed byseveral billion years due to residual feedback from stellar winds and Type Iasupernovae; even at $z=0$, the third galaxy remains in a temporary equilibriumwith a large gas content but without any ongoing star formation. Using the"genetic modification'' approach, we create an alternative mass growth historyfor this gas-rich quiescent dwarf and show how a small $(0.2\,\mathrm{dex})$increase in dynamical mass can overcome residual stellar feedback, re-ignitingstar formation. The interaction between feedback and mass build-up produces adiversity in the stellar ages and gas content of low-mass dwarfs, which will beprobed by combining next-generation HI and imaging surveys.

EDGE: From quiescent to gas-rich to star-forming low-mass dwarf galaxies