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Evolution of solar active regions (ARs) is directly related to the occurrence of flares and coronal mass ejections. In this sense, changes in AR magnetic field can be used to unveil other relevant features like plasma flows in the region and vertical Poynting flux into the overlying atmosphere. Here, surface 3D vector magnetic field observations from SDO/HMI are studied with the differential affine velocity estimator for vector magnetograms (DAVE4VM) to recover 3D plasma flows in the photosphere. From these results, the evolution of vertical Poynting flux is presented over the lifetimes of several ARs that display differing Mt. Wilson magnetic classifications.