New insight into lunar impact melt mobility from the LRO camera

Bray, V. J.; Tornabene, L. L.; Keszthelyi, L.; McEwen, A. S.; Hawke, B. R.; Giguere, T. A.; Kattenhorn, S. A.; Garry, W. B.; Rizk, B.; Caudill, C. M.; Gaddis, L. R.; Bogert, C. H. van der

doi:10.1029/2010gl044666

Cited by 98 publications

(64 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In general, the majority of the highly shocked and melt-rich materials preferentially remain in the original transient crater (e.g., Grieve et al, 1977), but volumes of these materials scale disproportionately with increasing transient cavity diameter (e.g., Cintala and Grieve, 1998). Consequently, as crater diameter increases, additional highly shocked and melt-rich deposits are emplaced both within and outside of the final crater, which is consistent with theoretical, numerical (Grieve and Cintala, 1992;Cintala and Grieve, 1998) and empirical observations (Hawke and Head, 1977;Cintala and Grieve, 1998;Bray et al, 2010;Osinski et al, 2011).…”

Section: An Impact Origin For Crater-related Pitted Materialssupporting

confidence: 74%

Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process

Tornabene

Osinski

McEwen

et al. 2012

Icarus

126

View full text Add to dashboard Cite

Section: An Impact Origin For Crater-related Pitted Materialssupporting

confidence: 74%

Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process

Tornabene

Osinski

McEwen

et al. 2012

Icarus

126

View full text Add to dashboard Cite

“…Most impact melts settle on impact crater floors, although some are ejected from the crater during the excavation stage, or pushed up and over the crater rim during the modification stage, followed by accumulation in topographic lows (e.g., Howard and Wilshire, 1975;Hawke and Head, 1977;Osinski et al, 2011). Morphologically impact melts can appear similar to some types of volcanic flows (i.e., lobate lava flows, sheet flows, and lava ponds: Howard and Wilshire, 1975;Hawke and Head, 1977;Bray et al, 2010;Carter et al, 2012;Denevi et al, 2012), although their source regions are traceable to impact craters rather than volcanic vents. Some of the highest resolution Lunar Reconnaissance Orbiter Camera-Narrow Angle Camera (LROC-NAC) images, however, show that lunar impact melts can have a highly variable texture, from smooth to rough at the meter scale to very rough at the decimeter scale (Carter et al, 2012).…”

Section: Impact Meltsmentioning

confidence: 99%

“…Lunar impact melt flows (Fig. 1) typically contain a variety of blocks transported by the partially-molten flow (Dence, 1971;Howard and Wilshire, 1975;Hawke and Head, 1977;Bray et al, 2010).…”

Section: Impact Meltsmentioning

confidence: 99%

Lobate and flow-like features on asteroid Vesta

Williams

O’Brien

Schenk

et al. 2014

Planetary and Space Science

View full text Add to dashboard Cite

a b s t r a c tWe studied high-resolution images of asteroid Vesta's surface ( $ 70 and 20-25 m/pixel) obtained during the High-and Low-Altitude Mapping Orbits (HAMO, LAMO) of NASA's Dawn mission to assess the formation mechanisms responsible for a variety of lobate, flow-like features observed across the surface. We searched for evidence of volcanic flows, based on prior mathematical modeling and the well-known basaltic nature of Vesta's crust, but no unequivocal morphologic evidence of ancient volcanic activity has thus far been identified. Rather, we find that all lobate, flow-like features on Vesta appear to be related either to impact or erosional processes. Morphologically distinct lobate features occur in and around impact craters, and most of these are interpreted as impact ejecta flows, or possibly flows of impact melt. Estimates of melt production from numerical models and scaling laws suggests that large craters like Marcia ( $ 60 km diameter) could have potentially produced impact melt volumes ranging from tens of millions of cubic meters to a few tens of cubic kilometers, which are relatively small volumes compared to similar-sized lunar craters, but which are consistent with putative impact melt features observed in Dawn images. There are also examples of lobate flows that trend downhill both inside and outside of crater rims and basin scarps, which are interpreted as the result of gravity-driven mass movements (slumps and landslides).

show abstract

“…This unit has deficiently developed terraces and has higher albedo than other parts of crater walls. When moving down slope, impact melts are thought to be both erosive and depositional (Bray et al, 2010). In Fig.9, we can see that impact melts erode into the walls deeply, but it is unclear if the erosion into the wall is mechanical or thermal, or a combination of the two.…”

Section: Crater Floor Unitsmentioning

confidence: 95%

Geological Mapping of Lunar Crater Lalande: Topographic Configuration, Morphology and Cratering Process

Ling

Zhang

et al. 2017

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

View full text Add to dashboard Cite

ABSTRACT:Highland crater Lalande (4.45°S, 8.63°W; D=23.4 km) is located on the PKT area of the lunar near side, southeast of Mare Insularum. It is a complex crater in Copernican era and has three distinguishing features: high silicic anomaly, highest Th abundance and special landforms on its floor. There are some low-relief bulges on the left of crater floor with regular circle or ellipse shapes. They are ~250 to 680 m wide and ~30 to 91 m high with maximum flank slopes >20°. There are two possible scenarios for the formation of these low-relief bulges which are impact melt products or young silicic volcanic eruptions. According to the absolute model ages of ejecta, melt ponds and hummocky floor, the ratio of diameter and depth, similar bugle features within other Copernican-aged craters and lack of volcanic source vents, we hypothesized that these low-relief bulges were most consistent with an origin of impact melts during the crater formation instead of small and young volcanic activities occurring on the crater floor. Based on Kaguya TC ortho-mosaic and DTM data produced by TC imagery in stereo, geological units and some linear features on the floor and wall of Lalande have been mapped. Eight geological units are organized by crater floor units: hummocky floor, central peak and low-relief bulges; and crater wall units: terraced walls, channeled and veneered walls, interior walls, mass wasting areas, blocky areas, and melt ponds. These geological units and linear features at Lalande provided us a chance to understand some details of the cratering process and elevation differences on the floor. We evaluated several possibilities to understand the potential causes for the observed elevation differences on the Lalande's floor. We proposed that late-stage wall collapse and subsidence due to melt cooling could be the possible causes of observed elevation differences on the floor.

show abstract

New insight into lunar impact melt mobility from the LRO camera

Cited by 98 publications

References 15 publications

Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process

Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process

Lobate and flow-like features on asteroid Vesta

Geological Mapping of Lunar Crater Lalande: Topographic Configuration, Morphology and Cratering Process

Contact Info

Product

Resources

About