Example of a possible evolution to produce a system like Kepler-10. The upper panel (a) depicts planetary semimajor axis and pericenter distance (﹩{a}_{i}[1-{e}_{i}]﹩), while the lower panel (b) shows that of inclinations. Due to secular chaos with the companions, planet Kepler-10b reaches ﹩{a}_{1}(1-{e}_{1}^{2})\lesssim 0.02\,\mathrm{au}﹩ after ∼5 Myr, at which time tidal damping (f-mode diffusion or equilibrium tides) can potentially shrink the orbit to a final period ≲1 day. At the moment that the planet reaches its maximum eccentricity (indicated by gray vertical lines), its inclination is also the highest (i ∼ 70°), while the eccentricities of planets c and d are low (≲0.05). The initial eccentricities and inclinations for planets c to f are assumed to be e = 0.12 and i = 7°, while higher values (e₁ = 0.22 and i₁ = 12°) are assumed for Kepler-10b, to speed up its chaotic diffusion.