There are eight craters where researchers have found moonrs. It appears that they are part of decision making processes within their craters through on-chain voting.
YOUR CHOICES, THEIR FATE
An ancient crater located in the central highlands. It is named after the Arab astronomer and scientist Muhammad ibn Jābir al-Harrānī al-Battānī, Latinized as Albategnius.
Albategnius is located to the south of the crater Hipparchus, to the east of Ptolemaeus and Alphonsus. The surface in this area is marked by a set of nearly parallel scars that form channels running roughly in a north–south line, bent slightly to the southeast.
Albategnius is located to the south of the crater Hipparchus, to the east of Ptolemaeus and Alphonsus. The surface in this area is marked by a set of nearly parallel scars that form channels running roughly in a north–south line, bent slightly to the southeast.
A crater that lies in the northwest part of the Moon’s near side. The crater is bright enough to be visible to the naked eye, and displays bright features when viewed through a large telescope. It’s also identified when most of the lunar surface is illuminated by earthshine. The crater is deeper than the Grand Canyon.
Aristarchus is located at the southeastern edge of the Aristarchus plateau, an elevated area that contains a number of volcanic features, such as sinuous rilles. This area is also noted for the large number of reported transient lunar phenomenas.
Aristarchus is located at the southeastern edge of the Aristarchus plateau, an elevated area that contains a number of volcanic features, such as sinuous rilles. This area is also noted for the large number of reported transient lunar phenomenas.
To the immediate south of Aristoteles lies the slightly smaller crater Eudoxus and these two form a distinctive pair for a telescope observer.
Observers have noted the crater wall of Aristoteles is slightly distorted into a rounded hexagon shape. The inner walls are wide and finely terraced. The outer ramparts display a generally radial structure of hillocks through the extensive blanket of ejecta. The crater floor is uneven and covered in hilly ripples.
Observers have noted the crater wall of Aristoteles is slightly distorted into a rounded hexagon shape. The inner walls are wide and finely terraced. The outer ramparts display a generally radial structure of hillocks through the extensive blanket of ejecta. The crater floor is uneven and covered in hilly ripples.
Bailly is a lunar impact crater that is located near the south-west limb of the Moon. The oblique viewing angle gives the crater a foreshortened appearance, and the location near the limb can limit visibility due to libration.
The most favorable time for viewing this feature is near the full moon when the terminator is crossing the crater wall.
The most favorable time for viewing this feature is near the full moon when the terminator is crossing the crater wall.
One of the largest formations on the Moon and the second largest crater on the visible near side. It is located in the rugged southern highlands of the Moon, to the south of the prominent ray crater Tycho.
It is one of the older formations on the lunar surface formed during the Nectarian period about 4 billion years ago. Despite its age the crater is relatively well-preserved. Water is trapped into tiny beadlike structures in the soil that form out of the high heat created by micrometeorite impacts.
It is one of the older formations on the lunar surface formed during the Nectarian period about 4 billion years ago. Despite its age the crater is relatively well-preserved. Water is trapped into tiny beadlike structures in the soil that form out of the high heat created by micrometeorite impacts.
Located in eastern Oceanus Procellarum. It typifies craters that formed during the Copernican period in that it has a prominent ray system. It may have been created by debris from the breakup of the parent body of asteroid 495 Eulalia 800 million years ago.
The crater rays spread as far as 800 kilometers across the surrounding mare. The rays are less distinct than the long, linear rays extending from Tycho, instead forming a nebulous pattern with plumy markings.
The crater rays spread as far as 800 kilometers across the surrounding mare. The rays are less distinct than the long, linear rays extending from Tycho, instead forming a nebulous pattern with plumy markings.
The worn remnant of a walled lunar plain. Located to the northeast of Mare Cognitum and southeast of Mare Insularum. Attached to the southern rim are the co-joined craters Bonpland and Parry, which intrude into the formation forming inward-bulging walls.
The floor of this formation has been covered by basaltic lava. This surface is divided by clefts running from the north and south rims. There is no central peak, the tiny crater Fra Mauro E lies at almost the midpoint of the formation.
The floor of this formation has been covered by basaltic lava. This surface is divided by clefts running from the north and south rims. There is no central peak, the tiny crater Fra Mauro E lies at almost the midpoint of the formation.
Located near the eastern lunar limb, the feature is circular in shape. It lies on the eastern shore of the Mare Fecunditatis. To the south is the overlapping crater pair Vendelinus and the smaller Lamé.
The inner wall is wide and irregularly terraced, with an average width of about 20 kilometers. The outer ramparts are irregular and hilly, and there is a bright, fragmented ray system spread across the mare to the west. The interior of the crater has a higher albedo than the surroundings, appearing bright when the Sun is overhead.
The inner wall is wide and irregularly terraced, with an average width of about 20 kilometers. The outer ramparts are irregular and hilly, and there is a bright, fragmented ray system spread across the mare to the west. The interior of the crater has a higher albedo than the surroundings, appearing bright when the Sun is overhead.