Abundance difference in this pair and other twin-like (Δ T_eff ≲ 100 K) wide binaries in Brewer et al. (2016). The differences in other pairs are small (<0.05 dex) for all elements except for ﹩{\rm{N}}﹩ and ﹩{\rm{O}}﹩, which are the most uncertain, making the difference of ≈0.2 dex seen in Kronos–Krios rare. Additionally, we show the distribution of the abundance differences between field stars with similar metallicity difference (﹩{\rm{\Delta }}[\mathrm{Fe}/{\rm{H}}]\approx 0.2﹩) as blue shaded regions. The widths of the shaded regions reflect the probability density as a function of ﹩{\rm{\Delta }}[{\rm{X}}/{\rm{H}}]﹩ for a given element, and the medians are indicated by the black line segments. These are random pairings of single stars in Brewer et al. (2016) at two metallicity bins, ﹩-0.025\lt [\mathrm{Fe}/{\rm{H}}]\lt 0.025﹩ (160 stars) and ﹩0.175\gt [\mathrm{Fe}/{\rm{H}}]\gt 0.225﹩ (137 stars), similar to Kronos and Krios. The difference is always taken to be ﹩\mathrm{higher}\,[\mathrm{Fe}/{\rm{H}}]-\mathrm{lower}\,[\mathrm{Fe}/{\rm{H}}]﹩. Thus, the narrower range of ﹩{\rm{\Delta }}[\mathrm{Fe}/{\rm{H}}]﹩ is by construction. Random pairings of disk stars with similar ﹩{\rm{\Delta }}[\mathrm{Fe}/{\rm{H}}]﹩ usually show a similar enhancement in all other elements, unlike the pattern seen in the Kronos–Krios pair.