Dynamic stability and instability behavior of Kepler-47 b depending on the initial binary eccentricity. The top panel represents the maximum difference between a_crit and a_cbp in its entire long-term evolution. If a_crit − a_cbp is less thanzero, the dynamic stability limit never engulfs Kepler-47b. The middle panel shows the time in which a_crit crosses into a_cbp (a_crit = a_cbp) during each simulation’s history. The maximum instability time is 33.6 Myr at e_bin = 0.236 and drops as the initial e_bin increases. The dashed vertical lines represent transitional values of e_bin. The bottom panel shows when each of the binary stars tidally lock during each simulation. Tidal lock time for the secondary star, Kepler-47B, is constant compared to the initial e_bin, however the tidal lock time for the more massive primary star, Kepler-47A, jumps from 69.3 Myr at e_bin = 0.19 to 3.93 Gyr at e_bin = 0.20 and decreases to zero as the initial e_bin increases. The approximate runtime was 42 h in total. github.com: cbp_dynamic_stability/K47_Eccentricities