Comparison of the predicted image at ν = 10¹¹ Hz using the average properties of the simulation (left) to the average of individual images computed for each snapshot of the simulation (right). For this figure, we used the a0SANE simulation with the parameters of the fiducial model. The striking difference between the images is due to the presence of short-lived, magnetically dominated filaments in the inner accretion flow, which contribute significantly to the emission in each snapshot but are washed out when computing the mean flow.