A hybrid simulation of the solar wind-Venus interaction and a test particle simulation of heavy ion trajectories near Venus are used to compute the contribution from solar wind charge exchange processes to the X-ray emission from Venus. It is found that the X-ray halo caused by the solar wind charge exchange process at Venus is confined to lower altitudes than at Mars, and that the structure on the ion gyro radius scale that is seen in X-ray images of Mars is absent at Venus.