Transient dynamical wormholes with decaying radial energy flux

We investigate a class of time-dependent traversable wormholes within the framework of general relativity by allowing the shape function to vary with time. In this setting, the evolution of the geometry is directly connected to a radial energy flux through the off-diagonal component of the Einstein field equations, providing a natural mechanism for non-static configurations. By adopting a decaying flux profile, we obtain exact solutions in which the geometry consists of a static background supplemented by a transient term that diminishes with time. The resulting spacetime satisfies the standard conditions required for a traversable wormhole, including the presence of a throat, the flaring-out condition, and asymptotic flatness. The corresponding matter content is determined explicitly and shows a clear temporal evolution governed by the decay parameter. An analysis of the energy conditions indicates that the null energy condition is violated in the vicinity of the throat, although the degree of violation decreases as the system evolves. This feature is examined further through a volume integral that measures the total amount of exotic matter, demonstrating that it approaches a constant value at late times. We also study the response of the system to small perturbations and find that, for a suitable choice of parameters, the configuration remains stable with perturbations decaying over time. We discuss how this flux-driven mechanism relates to the alternative and extensively studied approach in which wormhole evolution is instead carried by a cosmological scale factor, and we identify possible physical origins of the assumed radial flux in terms of null-fluid matter sources. Overall, the model describes a wormhole spacetime whose evolution is controlled by energy transport, leading to a gradual transition toward a static configuration. This framework offers a simple and physically motivated approach to dynamical wormholes and may be useful for exploring more realistic scenarios in both general relativity and extended theories of gravity.