In addition to its dominant central peak and pronounced wall terracing, this young complex crater displays a striking multilobate ejecta blanket that is common on Mars. (On Mars, craters greater than approximately 10 kilometers in diameter exhibit complex forms.) The favored model for the lobate ejecta pattern is through fluidized flow: Excavation and heating of ice in the target material causes a ground-hugging surge deposit, rather than aerial ejection along ballistic trajectories. The visibility of the preexisting crater just outside Yuty's rim indicates that these ejecta deposits are relatively thin.
Viking Orbiter image 003A07.