The critical densities and impact of forming ∆(1232) resonances in neutron stars are investigated within an extended nonlinear relativistic mean-field (RMF) model. The critical densities for the formation of four different charge states of ∆(1232) are found to depend differently on the separate kinetic and potential parts of nuclear symmetry energy, the first example of a microphysical property of neutron stars to do so. Moreover, they are sensitive to the in-medium Delta mass m∆ and the completely unknown ∆-ρ coupling strength gρ∆. In the universal baryon-meson coupling scheme where the respective ∆-meson and nucleon-meson coupling constants are assumed to be the same, the critical density for the first ∆ − (1232) to appear is found to be ρ crit ∆ − =(2.08 ± 0.02)ρ0 using RMF model parameters consistent with current constraints on all seven macroscopic parameters usually used to characterize the equation of state (EoS) of isospin-asymmetric nuclear matter (ANM) at saturation density ρ0. Moreover, the composition and the mass-radius relation of neutron stars are found to depend significantly on the values of the gρ∆ and m∆.