Near-surface ice on Mercury and the Moon: a topographic thermal model

The application of a thermal model to the high-latitude impact craters on the Moon and Mercury reveals that water-ice could have existed throughout the geological period in some of the craters. The Chao Meng Fu crater in Mercury, the floor of which is permanently devoid of sunlight, is capable of supporting water ice inside the crater walls. The unnamed bowl-shaped crater in Mercury is not capable of having water-ice, even though its floor is shadowed from direct sunlight because of its high temperature. Water ice could have existed in the Peary crater on the Moon due to the obliquity of the Moon.