\begin{document}$\psi$\end{document} evolves with time t, and its magnitude on the apparent horizon \begin{document}$|\psi_{\rm h}|$\end{document} starts from zero, undergoes a sharp rise followed by rapid oscillations, and eventually converges to a constant value. The variation in the photon sphere radius \begin{document}$r_{\rm ps}$\end{document} is similar to that of the magnitude \begin{document}$|\psi_{\rm h}|$\end{document}. Owing to the emergence of the complex scalar hair \begin{document}$\psi$\end{document}, the apparent horizon radius \begin{document}$r_{\rm h}$\end{document} starts increasing sharply and then smoothly approaches a stable value eventually. The shadow radius \begin{document}$R_{\rm sh}$\end{document} of the black hole with an accretion disk increases with time \begin{document}$t_{\rm o}$\end{document} at the observer's position. In the absence of an accretion disk, the shadow radius \begin{document}$R_{\rm sh}$\end{document} is larger and also increases as \begin{document}$t_{\rm o}$\end{document} increases. Furthermore, we slice the dynamical spacetime into spacelike hypersurfaces for all time points \begin{document}$t$\end{document}. For the case with an accretion disk, the variation in \begin{document}$R_{\rm sh}$\end{document} is similar to that in the apparent horizon \begin{document}$r_{\rm h}$\end{document}, because the inner edge of the accretion disk extends to the apparent horizon. In the absence of an accretion disk, the variation in \begin{document}$R_{\rm sh}$\end{document} is similar to that in the photon sphere radius \begin{document}$r_{\rm ps}$\end{document}, because the black hole shadow boundary is determined by the photon sphere. As the variation in \begin{document}$r_{\rm ps}$\end{document} is induced by \begin{document}$\psi$\end{document}, it can be stated that the variation in the size of the shadow is similarly caused by the change in \begin{document}$\psi$\end{document}. Regardless of the presence or absence of the accretion disk, the emergence of the complex scalar hair \begin{document}$\psi$\end{document} causes the radius \begin{document}$R_{\rm sh}$\end{document} of the shadow to start changing. Moreover, we investigate the time delay \begin{document}$\Delta t$\end{document} of light propagating from light sources to the observer. These findings not only enrich the theoretical models of dynamic black hole shadows but also provide a foundation for testing black hole spacetime dynamics."> Dynamic shadow of a black hole with a self-interacting massive complex scalar hair -
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