Solar prominences are cool and dense plasma suspended in the million-degree solar corona. Recent observations reveal that prominences are composed of fine and highly dynamic threads aligned with the local magnetic field. We have constructed a 3D time-dependent model of a prominence combining a magnetic field structure with 1D independent simulations of many flux tubes. The 3D magnetic field is taken from an adaptive MHD simulation of a sheared double-arcade filament channel. We use the thermal non-equilibrium model for the plasma evolution. We study different parametrization of the heating function, and with the results of our simulations we produce synthetic emission images of the whole prominence and the overlying loops. We show the evolving properties of our model and compare the results with data from telescope onboard satellites SOHO, STEREO, Hinode, and the recently launched SDO.