What is "schiaparelli"

Schiaparelli may refer to:

Schiaparelli is a lunar crater located on the western part of the Oceanus Procellarum, to the west of the crater Herodotus. The rim is relatively sharp-edged and relatively free from impact wear. The inner walls have slumped to form a shelf around much of the sides. The interior floor is somewhat irregular, but free from impacts of note.

This crater lies in a relatively flat and featureless part of the mare, although a ray streak from the distant crater Glushko passes along the southeastern edge of the rim, making it easy to identify. A low wrinkle ridge runs from the north rim of the crater to the north. Within the crater is a low central rise.

Schiaparelli (crater) may refer to:

• Schiaparelli (lunar crater)
• Schiaparelli (Martian crater)

Schiaparelli is an impact crater on Mars named after Giovanni Schiaparelli located near Mars's equator. It is in diameter and located at latitude 3° south and longitude 344°. A crater within Schiaparelli shows many layers that may have formed by the wind, volcanoes, or deposition under water.

Layers can be a few meters thick or tens of meters thick. Recent research on these layers suggests that ancient climate change on Mars, caused by regular variation in the planet's tilt, may have caused the patterns in layers. On Earth, similar changes (astronomical forcing) of climate results in ice-age cycles.

The regular appearance of rock layers suggests that regular changes in climate may be the root cause. Regular changes in climate may be due to variations of a planet's tilt (called obliquity). The tilt of the Earth's axis changes by only a little more than 2 degrees since our moon is relatively large. In contrast Mars's tilt varies by tens of degrees. When the tilt is low (current situation on Mars), the poles are the coldest places on the planet, while the equator is the warmest (as on Earth). This could cause gases in the atmosphere, like water and carbon dioxide, to migrate poleward, where they would freeze. When the obliquity is higher, the poles receive more sunlight, causing those materials to migrate away. When carbon dioxide moves from the Martian poles, the atmospheric pressure increases, possibly causing a difference in the ability of winds to transport and deposit sand. Also, with more water in the atmosphere sand grains may stick and cement together to form layers.