In this highly foreshortened view from Cassini, the moons Mimas and Epimetheus appear to loom over the rings. Mimas, the larger of the two, is in the foreground in this view. Its orbit around Saturn is tilted relative to the plane of the rings by one and a half degrees. While that’s a small angle, it’s the largest tilt or inclination of any of the inner moons of Saturn. As a result, Mimas’s gravity exerts perturbations on ring particles pulling them upward (or downward, depending on which side of the rings the Moon is on and which way you want to call up) out of the ring plane. These vertical perturbations are particularly strong at the location of vertical resonances where repeated perturbations add up in phase launching bending waves in the rings.
Image Credit: NASA/JPL/Space Science Institute. Click the picture to go to the Cassini imaging web site and see the picture in full resolution.
The outermost ring separate from the others is the F ring. This picture was taken from slightly above the ring plane, and the Sun is below the ring plane, so dusty rings like the F ring are particularly bright. The rest of the image shows the outer third or so of the A ring. Towards the very outer edge of the A ring is the narrow Keeler gap. The tiny moon Daphnis orbits within the Keeler gap and is barely visible together with ripples in the edge of the gap that it is producing that shows up as a bright arc. Further in is the broader Encke gap with two faint dust rings visible within it. The series of dark marks between the Encke gap and the edge of the A ring are density waves, mostly caused by the moons Pandora and Prometheus. Interior to the Encke gap (closer to Saturn) are two strong wave signatures. The outer one is a density wave and the inner one is the Mimas 5:3 bending wave (I’m 95% sure - I haven’t measured the positions on this image exactly).