Four examples illustrating the dependence among the final planetary state, the disk lifetime (T_d), and the duration of the outward migration ($T_d^{+}$) along with the different values of τ_a,i and ${\tau }_{a,i}^{+}$. In each case, the upper panel shows the evolution of the semimajor axis (a) with shadows representing the variation in the pericenter and apocenter distances, the middle panel displays the eccentricity, and the bottom panel illustrates the evolution of the resonant angle (R.A.) for the four-planet architecture. The color-code used is the same as in Figure 2. The estimated semimajor axes and eccentricities of the observed planets are indicated by horizontal lines on the right border, which match the corresponding planet colors. Panel (FM) represents the fiducial model for four planets with the parameters listed in Table 1. Panel (A) presents a scenario with a longer disk lifetime and outward-migration duration, with T_d = 6.00 Myr and $T_d^{+}=4.00$ Myr until a final time of 30 Myr. It considers the same values for τ_a,i and ${\tau }_{a,i}^{+}$ as in the fiducial model. Panel (B) displays a model where the migration timescales for the two innermost planets are set to 0 Myr, whilst the migration evolution is maintained for the two outermost planets, as could arise if an inner cavity were present. The values T_d and $T_d^{+}$ are set to 1.00 and 0.33 Myr, respectively. Panel (C) illustrates a model where the three innermost planets do not migrate, but only the outermost does inward.