Mars lacks an intrinsic magnetic field, allowing the solar wind and its embedded interplanetary magnetic field to directly interact with the planet’s dayside ionosphere. During this interaction, energy and momentum from the solar wind are transferred to ions escaping from the ionosphere. This transfer is governed by the structure of the electric field and current systems induced by the solar wind interaction. In a previous study, we mapped the spatial distribution of the energy transfer rate – i.e. the power exerted by the electric field to accelerate planetary ions – using amitis, a high-performance GPU-based hybrid plasma model. In the present study, we further decompose the contributions of different electric field components in Mars’ induced magnetosphere: the motional, Hall, and ambipolar terms, under typical solar wind and ionospheric conditions. Our results show that the motional electric field dominates the energy transfer process across most of the interaction region via mass loading. In particular, the direct energy transfer between the solar wind and planetary ions via the motional electric field is a fundamental characteristic of the Martian induced magnetosphere. The Hall term becomes significant at the base of planetary ion plumes, where magnetic field lines are highly bent and ion densities are elevated. We also find that the motional term contributes more to the energization of planetary ion species with a higher m/q ratio compared to the Hall term. The ambipolar term is generally weak, but it can transport newborn ions to higher altitudes, where they become subject to other electric field components. We illustrate the contributions of each electric field term by tracing their associated power along the trajectories of test particles.