\begin{document}$f(\phi)={\rm e}^{-b\phi^2}$\end{document}, which facilitates both scalar-free RN and scalarized black hole solutions. We first present the evolution of system parameters during dynamic scalarization. For parameter regions in which spontaneous scalarization occurs, we observe that the evolution of the scalar field at the horizon is dominated by the fundamental unstable mode from linear analysis at early times. At late times, the nonlinear evolution can be considered to be the perturbation of scalarized black holes."> Dynamical spontaneous scalarization in Einstein-Maxwell-scalar theory -
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