Dynamical evolution of charged anisotropic compact stars: From static solutions to gravitational collapse

We investigate the radial evolution of charged anisotropic compact-star configurations within the spherically symmetric Einstein–Maxwell system using a corrected Misner–Sharp formulation. The charged mass aspect, initial radial metric, and local apparent-horizon condition consistently include the electromagnetic contribution q 2 / R 2 . The closed dynamical system evolves the areal radius, shell velocity, density, and mass, while the charge enclosed by each comoving shell is conserved. A linear radial equation of state and a regular anisotropy prescription complete the matter model and enforce p t = p r at the center. The selected finite-time calculations exhibit three characteristic behaviors: local apparent-horizon formation, bounded oscillatory motion over the simulated interval, and outward expansion up to the numerical stopping condition. Electric charge and positive anisotropy provide additional support against contraction, whereas negative anisotropy acts inward and promotes collapse. Alternative charge profiles are normalized to the same total charge, and grid-refinement and constraint monitoring provide numerical consistency checks. The documented configurations form a limited exploratory sample rather than a complete charge–anisotropy phase diagram. The calculations do not establish complete dispersal, nonlinear remnant stability, singularity avoidance, or a violation of cosmic censorship. Moreover, exact spherical symmetry produces no tensor gravitational radiation; therefore, no waveform, strain amplitude, or gravitational-wave detectability claim is made.