Wooo big basins!

Better-characterizing the formation of large impact basins like Orientale can provide unprecedented insight into conditions on the early Moon - and that includes new images of the basin from Artemis II! There's still lots to learn about why multi-ring basins form.

This 3D rendering of Orientale shows the terrain in high relief, as it would be just after sunrise. Gravity anomalies measured by the Gravity Recovery and Interior Laboratory (GRAIL) mission are depicted in different colors on the right side of the image. Red indicates areas of higher gravity, or excess mass, and blue indicates lower gravity or areas of mass deficits. The GRAIL data reveals the structure of the basin beneath the surface. The red in the center of the basin, for example, shows that the crust is particularly thin there, and that denser mantle material is closer to the surface. NASA's Scientific Visualization Studio

The intense deformation during and after the impact extended to the subsurface, leaving Orientale with a unique "bulls-eye" pattern of gravity anomalies, corresponding to excess mass (red) and mass deficits (blue).

None of Orientale's rings are the initial crater itself, which would fall somewhere between the two innermost rings. The initial transient crater formed by the impact would have been obliterated by subsequent deformation, which would have included extensive rebounding of material inside the crater.

The Orientale basin is the youngest of the large lunar basins. The distinct outer ring is about 590 miles (950 km) from east-to-west.

Orientale, the multi-ring impact basin that's a focus of Artemis II, is unique as the youngest of the Moon's large impact basins! Orientale's multiple rings are thought to have formed from deformation of the lunar crust and upper mantle in response to impact, generating circumferential ring faults.

Pedestal crater on Mars, as seen by HiRISE under HiWish program. Top layer has protected the lower material from being eroded. The location is Casius quadrangle.

Another pedestal crater on Mars, as seen by HiRISE under HiWish program Location is Hellas quadrangle.

Pedestal crater on Mars, as seen by HiRISE under HiWish program The ejecta is not symmetrical around crater because the asteroid came at a low angle out of the northeast, so there is an exclusion zone of no ejecta in that quadrant. The location is Casius quadrangle.

Pedestal crater on Mars, as seen by HiRISE under HiWish program Scallops are forming at the bottom edge of the pedestal. Location is Casius quadrangle.

Crater Fact Friday: there's lots of unusual types of craters across the Solar System! One of our favorite types is pedestal craters, which have ejecta blankets that sit above the surrounding terrain, forming a raised platform (like a pedestal). Many of these can be found on Mars.

Map of the overall resource potential of frozen materials in lunar PSRs. North (left) and south (right) pole PSR volatile ranking thematic maps overlaying Diviner Lunar Radiometer Experiment annual maximum bolometric temperature.

Permanently-shadowed craters can reach temperatures of -248 deg C, and the cumulative area of these craters is ~31 thousand km^2, which is more than half of the southern hemisphere!

English: Shackleton Crater in the Lunar South Pole region, mosaic created by LROC (Lunar Reconnaissance Orbiter) and ShadowCam teams.

Shackleton, Shoemaker, and de Gerlache crater as imaged by Earth-based radar.

The Artemis Base Camp concept is located near Shackleton and de Gerlache craters, two permanently-shadowed craters that future Artemis crews might be able to use for resources. The ice hidden in the Moon's eternal darkness can be used for drinkable water, breathable oxygen, and rocket fuel!

Erlanger is a very deep lunar impact crater that lies near the north pole of the Moon. Image taken by the Lunar Reconnaissance Orbiter Narrow Angle Camera.

One of the major focuses of future Artemis missions is landing on the lunar south pole near permanently shadowed craters. These types of craters are unique, as their locations near the poles of the Moon mean that - as the name implies - some portion of their interior is always in darkness.

Whose excited for the Artemis II launch?! 🚀

Artemis II mission is about to fly humans to the Moon — here’s the science they’ll do Set to lift off this week, the NASA flight will take astronauts around the Moon for the first time in more than 50 years.

Need to catch up on #ArtemisII science ahead of today's launch attempt to the MOON? See our explainer at @nature.com 🧪🔭

www.nature.com/articles/d41...

Image of a large impact crater on the moon with a central peak

We also love Copernicus!

Okay what about Linńe!?

What a beautiful looking impact basin on the top right! (Her name is Gertrude if you’re wondering!)

This is the biggest impact crater of the Uranian satellites, measuring at ~325 km in diameter.

correct!

Really lucky miss!

A four panel image showing different impact craters on various solar system bodies

Crater Fact Friday ☄️DID YOU KNOW☄️ impact cratering is the most ubiquitous surface process in the solar system? We see impact craters on almost every solid surface body (with *maybe* the exception of Io!)

Can you guess where these impact craters formed?

We are delighted to be here and look forward to sharing more about impacts ☄️ And we will even do our best to make crater counting fun!

The Planetary Crater Consortium (PCC) was originally established in 1998 as the Mars Crater Consortium. In 2010 PCC was formed as we aimed to facilitate collaborations between planetary scientists interested in any aspect of impact craters on solar system bodies (planets🌏moons🌗 asteroids☄️ comets!)

You can also sign up for our mailing list here: groups.google.com/g/planetary-...

The original PCC team from 2007 stands outside in Flagstaff, AZ.

Hello! 👋 We are the Planetary Cratering Consortium, a community-led organization of planetary scientists interested in all aspects of impact cratering. Follow us for up-to-date info about cratering news, fun crater facts, and upcoming meetings ☄️