Dynamical evolution of multi-planet systems from Table 2. Each column displays the evolution of stellar obliquities and mutual planetary inclinations for a system under two distinct initial stellar obliquity angles (ψ_⋆0). The magenta curves in each obliquity panel represent the evolution paths of equilibria. Note that in all simulations, we ignore the evolution of the eccentricity vectors by assuming all the orbits are initially circular. In addition to the parameters given in Table 2, other integration parameters are: m_⋆ = 1M_⊙, τ_d = 1 × 10⁴ yr, r_in = 0.03 au, and r_out = 50 au. The disk mass (m_d) is set to 0.05M_⊙ for Cases I-III and to 0.02M_⊙ for Case V, respectively.