Critical rotation rate Ω_K,diff of the dwarf galaxy as a function of the disk scale height H, as given in Eq. (34), to distinguish between the regime of low star formation and high rotation and the regime of low star formation and low rotation. In the former regime, we still expect a valid but steeper far-infrared − radio correlation, while in the limit of low rotation, the correlation between star formation and the magnetic field will break down before cosmic-ray diffusion becomes relevant. The critical rotation rate adopted here implicitly assumes observations at 1 GHz due to the diffusion timescale of the cosmic rays. Observations at higher frequencies will probe more energetic electrons, implying shorter diffusion times and a higher critical rotation rate.