LROC: Lunar landslides!

Low-reflectance granular material flowed down the northeastern wall of an unnamed crater and formed interweaved tendrils. LROC Narrow Angle Camera (NAC) observation M169398317R, LRO orbit 10,098, August 31, 2011; downslope is to the lower left, image field of view is 290 meters. (View the full 500 meter field of view in the LROC Featured Image HERE [NASA/GSFC/Arizona State University].

Lillian Ostrach
LROC News System

Although LROC collects images of craters on the lunar surface at only one moment in time, impact craters are not as static and unchanging as these images may lead you to believe. The majority of material movement occurs during the impact event over a very short time, sometimes lasting only a few seconds, but post-impact modification plays a large role in crater erosion over time. In fact, post-impact modification begins immediately after the crater is formed! Wall slumping that forms terraces or debris piles on the crater floor and solidification of impact melt ponds and flows are just two examples of modifications that begin soon after a crater is formed. Over historical time (one year, ten years, 100 years) as well as geologic time (tens to hundreds of millions of years), crater modification proceeds to degrade the pristine crater into a shallower, less-distinct crater (you can see some of these types of craters in the WAC context image below).

Crop from LROC Wide Angle Camera (WAC) monochrome (643 nm) observation M118695906ME, LRO orbit 2626, January 26, 2010 of the 44 km-wide crater Virtanen (below, near 15.80°N, 177.39°E) and the unnamed crater that impacted into its eastern wall, a scene from the middle latitudes of the lunar farside. From 54 kilometers overhead the scene does not capture a fell for the slope angles of the topography in this terrain as well as the false-color images built up from LOLA laser altimetry further below. The location of the scenes in the unnamed crater's inner walls are noted by the two blue arrows; the lower arrow notes the location of an additional explanatory close-up further down in this posting (the crater at the top of the image above is Virtanen Z). [NASA/GSFC/Arizona State University].

At Virtanen's equatorial latitudes laser altimeter observations are not as tightly bunched as they are nearer to lunar poles, where sequential polar orbital paths intersect as the Moon continuously rotates eastward below LRO's path relative to the lunar surface. This accounts for the ribbon-like texture to this topography, looking north-northeastward over Virtanen. Even so, at this oblique virtual perspective the true steep slope of the inside walls of the highlighted unnamed crater notched into Virtanen's east is very apparent, a difference of 7 kilometers in elevation from the crater rim to crater floor [NASA/LOLA/LMMP].

Today's Featured Image highlights a granular debris flow that originated near the crater rim and flowed downhill from the northeastern wall of an unnamed crater within Virtanen crater (15.80°N, 177.39°E). Along the way, the dry particles were disturbed by boulders that deflected the material. In a previous post, a boulder acted as a dam to stop the debris from flowing and created a "flow shadow" where the low-reflectance material did not reach - similar to what is visible here. However, in some cases, there is space between the boulder and the location at which the debris forks for its detour. Why might this be? Here's a hint: take a look at these boulders - do any of them have boulder trails or do they look like they are eroding out of the crater wall itself? There are no visible boulder trails, and the boulders of variable sizes are not sitting on the crater wall surface. In fact, most of the boulders look partially buried. So, it is likely that the low-reflectance granular material deflected around these boulders because the boulders are eroding out of the wall material and represent a small topographical high compared to the smoother, unbouldered portion of the crater wall. What do you think?

LROC WAC monochrome mosaic from 5 orbital observation opportunities in January 2010, including M118695906ME shows the Virtanen crater group, Buys-Ballot, etc. are superimposed features on the wide floor of a highly eroded, but still distinct basin; actually within at least two distinct mountainous rings (see the LOLA hemisphere-wide false color image, centered on Virtanen, below  [NASA/GSFC/Arizona State University].

A small white arrow notes the location of Virtanen, well inside a 650 km-wide basin as mapped by LRO's LOLA, over the course of the past two years [NASA/LOLA/LMMP].

The southeastern crater wall near the crater rim (below) is markedly different than the northeastern part of the crater wall nearing the crater floor (opening image). Instead of well-developed low-reflectance debris flows tendrils located downhill from the crater rim because of gravity, there is a mix of both high- and low-reflectance material on the crater wall slope. There are also large erosional troughs or alcoves from which the material forming debris flows originates. The contrast between reflectance of the crater wall and the lower-reflectance material traveling downslope (to the upper left) illustrates that the crater wall is not a smooth, flat surface. Small slope breaks in the crater wall acted as a dam to halt debris on their downward descent to the crater floor. Maybe these troughs will erode to the point where, in several millions of years, substantial material from the upper part of the southeastern wall will have mobilized downhill to form debris flows similar to those on the northeastern slope.

The southeastern crater wall has deep alcoves from which material erodes. LROC NAC M169398317R, illumination is from the bottom/bottom left, image width is 290 meters [NASA/GSFC/Arizona State University].

Explore these debris flows from the comfort of your computer seat in the full LROC NAC image!

Related posts:
Dichotomy
Tendrils in Reiner Crater
Erosional trough on crater wall
Rock avalanche in Robinson crater
Granular Flow

It's the Moon's fault

Linear rille in Mare Tranquillitatis, the result of extensional stresses. What caused the offset in the rille on the east wall? LROC Narrow Angle Camera (NAC) observation M146858595LE, LRO orbit 6776, December 13, 2010, field of view 700 meters. See the full size LROC Featured Image HERE [NASA/GSFC/Arizona State University].

Drew Enns
LROC News System

Linear rilles are so named because of their nearly-straight morphology and surface expression. Unlike sinuous rilles, which are volcanic, linear rilles are tectonic in nature. Similar features on Earth are termed graben, and are created when two normal faults border a block of rock which has been depressed, producing a valley.

Since normal faults are understood to be the products of extensional stresses (see yesterday's Featured Image post), we can assume this region of the Moon was "pulled apart" - creating these normal faults, dropping the middle blocks, and producing the linear rilles. So a linear rille is the lunar analog of a graben on Earth!

Full two kilometer width segment of LROC NAC frame M146858595LE, showing the approximate location of the LROC Featured Image, September 15, 2011 [NASA/GSFC/Arizona State University].

LROC Wide Angle Camera (WAC) context images of the Rimae Sosigenes extensional linear rille system in the northeast Mare Tranquillitatis, between the Arago domes (out of view, to the south and east) and the craters Sosigenes and its smaller namesake Sosigenes A. one rille is cross-cut with a close-grouped and prominent secondary crater chain, well-known to well-equipped telescopic observers when the morning terminator passes over five days following a New Moon. WAC monochrome (566 nm) mosaic from orbits 4515-4517, June 18, 2010. See the original LROC WAC context image HERE [NASA/GSFC/Arizona State University].

In today's featured image, two normal faults appear to be offset.

What are we seeing here?

Is Mare Tranquillitatis really an impact basin? Looks can be deceiving, when comparing two familiar and neighboring basins, each flooded multiple times with volcanic flows. Dark and optically-mature regolith covers both Mare Serenitatis (top center) and Tranquillitatis (below - the area of interest is indicated with the yellow area), though the differences in color of each are obvious even in black and white photographs. But In this false-color LOLA elevation map, the nature of Mare Tranquillitatis is less obvious, until one examines more closely and sees how the weight of material infilling the Tranquillitatis plain may have led to finer features like wrinkle ridges and extensional rilles [NASA/GSFC/LOLA/MSFC/LMMP].

It is probably an en echelon step between the two normal faults making up the east wall of the rille. When two faults are near to each other, they can interact and create an en echelon step that helps to even out the displacement and forces that created the faults. En echelon steps are common, and are seen in other tectonic features on the Moon.

Can you find any more faults in the full NAC frame?

Related Posts:
Rima Bürg
Rima Ariadaeus - A Linear Rille

LOLA: refining impact basin dimensions

Laser altimetry by LOLA, now having traveled nearly 10,000 orbits of the Moon on-board the Lunar Reconnaissance Orbiter, has confirmed the existence of impact basins once believed "questionable" [NASA/GSFC].

GSFC - This image reveals the power LOLA data have in helping scientists refine sizes of impact basins on the Moon. By studying lunar impact basins, scientists refine their understanding of what happened in the earliest stages of the formation of our Solar System, including the size distribution of early impactors.

The Sikorsky-Rittenhouse impact basin, which is estimated to be between 3.9 and 3.5 billion years old, was originally estimated to be 310 km in diameter, and its existence was considered "questionable" in Wilhelms' lunar atlas.

The ghostly Sikorsky-Rittenhouse impact basin, northwest its more-recent doppelganger, the slightly larger and still well-defined Schrodinger basin, is also visible in this LROC Wide-Angle Camera (LROC WAC WMS) global mosaic [NASA/GSFC/Arizona State University].

This initial definition was based on low-resolution images from Lunar Orbiter missions. Later Earth-based radar estimates confirmed Sikorsky-Rittenhouse's status as a basin and placed the basin diameter at 319 km. However, the use of LOLA data have helped scientists to further define the diameter size to 275 km, which represents an 11% decrease in the original diameter estimate. LOLA's high density of measurements across the Moon allows its data to create the most accurate definition of lunar craters ever.

References:

1. Jones, N. and B. Steigerwald, (2010) "NASA's LRO Exposes Moon's Complex, Turbulent Youth," 03 June 2011.
2. Wilhelms, D.E, (1987) The Geologic History of the Moon, USGS Professional Paper 1348
3. Frey, H.V. (2010) Chapter 2, GSA Special Publication Recent Advances and Current Research Issues in Lunar Stratigraphy (in press).
4. Romine, G.C., and H.V. Frey, (2011) "Using LOLA Data to Test the Reality of Candidate Lunar Basins Derived from Older Data," 41st Lunar and Planetary Science Conference, Abstract 1188, March 1-5, The Woodlands, TX.

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Late in its mission, Japan's Kaguya captured this relatively low altitude HDTV view across 98 km-wide Sikorsky (66.1°S, 103.2°E), bisected by 310 km-long Vallis Schrodinger. The northern rim, where the horns of the Valley cross through, is also the broader and essentially invisible rim of the Sikorsky-Rittenhouse impact basin. View the full-sized Kaguya HDTV image HERE [JAXA/NHK/SELENE].