Impact of the small-scale magnetic fields of Rempel’s (2014) model on the determination of the solar iron abundance. Top panel: corrections of the Fe i abundances due to the direct Zeeman broadening effect on the Fe i lines. Middle panel: corrections of the Fe i abundances caused by the magnetically induced changes of thermodynamical properties of the solar photosphere in the line formation regions. Bottom panel: combined effect representing the sum of the ΔA values shown in the top and middle panels. The abundance corrections are given against the mean line-center optical depths of the Fe i lines calculated in the 3D model snapshot with ⟨ | B_z | ⟩ = 0.5 G. The mean of the abundance corrections, ⟨ ΔA ⟩, and their corresponding rms values are shown in the upper left corner of each panel.