Study in superpositioning at Vavilov D

Sunrise, sunset. LROC NAC observations 10 months apart, one at local sunset and the other after local sunrise, both from nearly identical altitudes and resolutions, capture these views of double "dingleberries," drops of hot melt, very likely from the impact that created Vavilov crater, sit where they quickly flattened and cooled, just inside the steep slope of ancient Vavilov D. The Vavilov craters are a study in stratigraphy and superposition [NASA/GSFC/Arizona State University].

Immediately inside the northwest rim of highly degraded Vavilov D, twin disks of impact melt, likely from the formation of Vavilov, came to a standstill at the upper end of a contiguous slope of 5000 meters elevation, over about 40 km, into the complex floor of the latter Eratosthenian crater. This 1400 meter field of view (down slope is to the lower right, centered on 1.14°N, 221.536°E) from LROC NAC observation M1128031686L, LRO orbit 18385, July 9, 2013; 61° incidence angle, resolution 1.17 meters from 114.6 km [NASA/GSFC/Arizona State University]. 

Hiroyuki Sato

LROC News System

Vavilov D is an heavily degraded crater (96.1 km; 0.026°N, 220.93°E) sits between the Orientale basin and Jackson crater, both of which it may pre-date.

The later formation of the nearly identical, over-lapping Vavilov crater (98.2 km; 0.87°S, 221.23°E) eradicated the entire southwestern half of Vavilov D.

The second image above spotlights a spot on the northwestern curve of the wall of Vavilov D near where the Eratosthenian Vavilov erased the older crater's anatomy. The relatively smooth textured area in the upper left corresponds to the outside of Vavilov D, and the rest of rough/craggy surface is the interior crater wall's steep slope. 

The two degraded craters (~280 m in diameter) near the middle of the opening image exhibit fascinating overlying smooth features that may have formed as material flowed downslope (arrows).

View the full-resolution original HERE. The twin melt disks are located where the rim of Vavilov superseded that of Vavilov D, in the farside equatorial highlands,  where Vavilov is etched into terrain 8000 meters above the global mean elevation. It's possible an astronaut could walk from this location south into the interior of Vavilov. 5.6 km-wide field of view from LROC NAC observation M1128031686L [NASA/GSFC/Arizona State University].

Other morphologic pits/dents on this slope also have similar textures. What we are seeing here are most likely remnant impact melt that was thrown out of the Vavilov crater. Craggy sloped surfaces with patches of smooth material are often found associated with young impact craters -- formed as impact melt flowed over and around the newly formed crater.

The deepest material brought to the surface by impacts on the Moon is found on the resulting crater's rim. A fresh crater near our area of interest, on the rim of Vavilov D (cross), exposes material excavated by that ancient impact, and Vavilov D, in turn, is nested on the Hertzsprung basin. The larger region is also at the outside range of the majority of secondary craters from the Orientale basin-forming impact. LROC Quickmap mosaic [NASA/GSFC/Arizona State University].

Depth of field in lunar photography is a fleeting quality. With the LROC WAC-derived elevation model (GLD100), however, the super-positioning of Vavilov D (and an aeon or two later, Vavilov) on Hertzsprung is much easier to detect, along with some of the most extreme elevation ranges, some 9 km above the global mean [NASA/GSFC/DLR/Arizona State University].

Related Posts:

View from Vavilov
Craggy Peak, Impact Melts
Rough Crater Wall Surface
Sinuous Cracks
View From The Other Side
Dark Impact Melt Sheet
Fractured Melt Rock
Young Crater Walls

Overprinting Orientale

Fractured crater draped with ejecta from the impact event that created the Orientale basin, south of Buffon crater (downslope to the right). Crop from LROC NAC oblique mosaic M1128039712LR, LRO orbit 18386, July 9, 2013; 74.2° angle of incidence, resolution very roughly 2.3 meters, spacecraft and camera slewed 65.27° toward the east, from 58.43 km over 46°S, 222.48°E  [NASA/GSFC/Arizona State University].

J. Stopar
LROC News System

This spectacular oblique view looks from west to east across an area south of Buffon crater (45.715°S, 229.052°E) that is draped with impact ejecta from the Orientale Basin.

Orientale ejecta to have flowed over a pair of modified craters (each approximately 16 km in diameter, also see image at far bottom). Because the ejecta is superposed on top of the craters and appears to flow over much of the scene, the ejecta should be younger than the craters. However, these craters do not exhibit typical morphologies, and neither does the Orientale ejecta! Just how did this spectacular scene form?

Full width NAC oblique image of Orientale ejecta covering the local terrain. Ejecta and crater floors are lumpy and crisscrossed by numerous graben. A flat lying mare pond is located just below center on the right side of the image (arrow). Scene is approximately 41 km in height, oblique view, west to east. Click image or HERE to view larger image [NASA/GSFC/Arizona State University].

First, the pair of prominent craters seen above have concentric, mounded or lumpy looking floors. This morphology is atypical of impact craters of this size (see Steno Q or Burg crater for more typical examples), but is reminiscent of many floor-fractured craters (such as Atlas or Komarov), which are thought to form through uplift caused by magma intruding deep beneath the surface. However, the graben seen in the examples above are more subdued those in most floor-fractured craters, suggesting that they may be blanketed by the overlying Orientale ejecta.

There is also a small pond of basalt (darker and flat) exposed just below the center on the right side of the full width image (above). This is a tell-tale sign of volcanic activity in the area, lending support to the hypothesis that the lumpy craters were modified by magma from below. This, however, does not prove which occurred first: the volcanism or the emplacement of the Orientale ejecta.

LROC Wide Angle Camera (WAC) mosaic of the area south of Buffon crater. Blue polygon highlights approximate boundaries of the area shown in the featured oblique Narrow Angle Camera (NAC) frame; arrow indicates location of impact melt flow featured in a previous post. The ejecta within the blue polygon is fractured and warped, but the ejecta indicated by the arrow is not [NASA/GSFC/Arizona State University].

The final observation that informs the sequence of events is the occurrence of similar graben in both the crater floors and the adjacent ejecta outside the craters that is not typical of Orientale ejecta in this region. The previous post Stopped in its Tracks featured a nearby Orientale ejecta deposit located only 30 kilometers west of today's spectacular image; that ejecta is not crisscrossed by graben like those seen in the opening image above! Thus, volcanic activity in this area may have occurred after the large impact event that formed the Orientale basin around 3.8 billion years ago. However, further analysis and age dating in this area are needed before we can say for certain that the Orientale ejecta was modified (or overprinted) by younger volcanism.

Detail of Orientale ejecta, showing inferred direction of flow towards the mare unit shown in the larger images above [NASA/GSFC/Arizona State University].

Try to unravel the sequence of events on display in the full oblique image, HERE.

Related Posts:
Ground Hugging Ejecta
Fall Out
Orientale Sculpture
The Fractured Floor of Compton
A Colorful History of Floor-Fractured Komarov