Extracting accurate and precise topography from LROC narrow angle camera stereo observations

Henriksen, M. R.; Manheim, M. R.; Burns, K. N.; Seymour, P.; Speyerer, E. J.; Deran, A.; Boyd, A. K.; Howington-Kraus, E.; Rosiek, M. R.; Archinal, B. A.; Robinson, M. S.

doi:10.1016/j.icarus.2016.05.012

Cited by 84 publications

(64 citation statements)

References 26 publications

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“…Topographic and slope analyses are conducted on a 2 m grid digital terrain model (DTM) produced from LROC NAC image pairs (Henriksen et al. ). SELENE‐TC+LRO‐LOLA merged DEM products (SLDEM2015; Barker et al.…”

Section: Methodsmentioning

confidence: 99%

The role of substrate characteristics in producing anomalously young crater retention ages in volcanic deposits on the Moon: Morphology, topography, subresolution roughness, and mode of emplacement of the Sosigenes lunar irregular mare patch

Qiao

Head

Xiao

et al. 2017

Meteorit & Planetary Scien

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Lunar irregular mare patches (IMPs) comprise dozens of small, distinctive, and enigmatic lunar mare features. Characterized by their irregular shapes, well‐preserved state of relief, apparent optical immaturity, and few superposed impact craters, IMPs are interpreted to have been formed or modified geologically very recently (<~100 Ma; Braden et al. ). However, their apparent relatively recent formation/modification dates and emplacement mechanisms are debated. We focus in detail on one of the major IMPs, Sosigenes, located in western Mare Tranquillitatis, and dated by Braden et al. () at ~18 Ma. The Sosigenes IMP occurs on the floor of an elongate pit crater interpreted to represent the surface manifestation of magmatic dike propagation from the lunar mantle during the mare basalt emplacement era billions of years ago. The floor of the pit crater is characterized by three morphologic units typical of several other IMPs, i.e., (1) bulbous mounds 5–10 m higher than the adjacent floor units, with unusually young crater retention ages, meters thick regolith, and slightly smaller subresolution roughness than typical mature lunar regolith; (2) a lower hummocky unit mantled by a very thin regolith and significantly smaller subresolution roughness; and (3) a lower blocky unit composed of fresh boulder fields with individual meter‐scale boulders and rough subresolution surface texture. Using new volcanological interpretations for the ascent and eruption of magma in dikes, and dike degassing and extrusion behavior in the final stages of dike closure, we interpret the three units to be related to the late‐stage behavior of an ancient dike emplacement event. Following the initial dike emplacement and collapse of the pit crater, the floor of the pit crater was flooded by the latest‐stage magma. The low rise rate of the magma in the terminal stages of the dike emplacement event favored flooding of the pit crater floor to form a lava lake, and CO gas bubble coalescence initiated a strombolian phase disrupting the cooling lava lake surface. This phase produced a very rough and highly porous (with both vesicularity and macroporosity) lava lake surface as the lake surface cooled. In the terminal stage of the eruption, dike closure with no addition of magma from depth caused the last magma reaching shallow levels to produce viscous magmatic foam due to H2O gas exsolution. This magmatic foam was extruded through cracks in the lava lake crust to produce the bulbous mounds. We interpret all of these activities to have taken place in the terminal stages of the dike emplacement event billions of years ago. We attribute the unusual physical properties of the mounds and floor units (anomalously young ages, unusual morphology, relative immaturity, and blockiness) to be due to the unusual physical properties of the substrate produced during the waning stages of a dike emplacement event in a pit crater. The unique physical properties of the mounds (magmatic foams) and hummocky units (small vesicles and large void space) altered the...

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Section: Methodsmentioning

confidence: 99%

The role of substrate characteristics in producing anomalously young crater retention ages in volcanic deposits on the Moon: Morphology, topography, subresolution roughness, and mode of emplacement of the Sosigenes lunar irregular mare patch

Qiao

Head

Xiao

et al. 2017

Meteorit & Planetary Scien

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“…2a) and a DTM mosaic of image pairs M150361817 and M150368601 ( Fig. 2b) (Henriksen et al, 2016). The NAC DTM shows a lowest elevation of -2017 m and a highest elevation of -1808 m. An orthographic projection (Longitude of the center: 23.6 and Latitude of the Center 0.69) was used for our study to minimize distortions (Anderson et al, 2004;Robinson et al, 2010).…”

Section: Datamentioning

confidence: 99%

Geological mapping and chronology of lunar landing sites: Apollo 11

Iqbal

Hiesinger

Bogert

2019

Icarus

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“…Cauchy 5 small shield volcano mapped by LROC NAC: (a) LROC NAC image (frame M1108025067, 1.2 m/pixel), (b) LROC NAC DTM topography (5 m/ pixel;Robinson et al, 2010;Henriksen et al, 2017), (c) NAC DTM-derived slope map (15 m baseline) and (d) 5 m contour interval map. All the images of the Cauchy 5 feature in this work are in a sinusoidal projection centered at 37.592°E, and north is up.…”

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The Cauchy 5 Small, Low‐Volume Lunar Shield Volcano: Evidence for Volatile Exsolution‐Eruption Patterns and Type 1/Type 2 Hybrid Irregular Mare Patch Formation

et al. 2020

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The lunar shield volcano Cauchy 5, sitting at the low diameter‐height‐volume end of the population, is the only known example containing two different types of Irregular Mare Patches (IMPs) in very close association: (1) the pit crater interior Type 1 IMP composed of bleb‐like mounds surrounded by a hummocky and blocky floor unit and (2) Type 2 IMPs, small, often optically immature pits less than ~5 m deep, located on the generally block‐deficient shield flanks. A four‐phase lunar magma ascent/eruption model predicts that during a relatively brief eruption, low magma rise rates maximize volatile exsolution in lava filling the pit crater. Bubble‐rich magmas overtop the pit crater and form extremely vesicular flows on the shield flanks. Exposure of the flanking flows to vacuum produces a fragmental layer of exploded glassy bubble walls. Subsequent second boiling upon cooling of the flanking flow interiors releases additional volatiles which migrate and collect, forming magmatic foams and gas pockets. As magma rise rates slow, trapped gas and magmatic foam build up below the cooling pit crater floor. Magmatic foams are extruded to form Type 1 IMP deposits. Type 2 IMPs on the flanks are interpreted to be due primarily to subsequent impacts causing collapse of the flow surface layer into the extremely vesicle‐ and void‐rich flow interior. Anomalously young pit crater floor/shield flank crater retention ages compared with surrounding maria ages may be due to effects of Cauchy 5 substrate characteristics (extreme micro‐ and macroporosity, foamy nature, and glassy auto‐regolith) on superposed crater formation and retention.

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Extracting accurate and precise topography from LROC narrow angle camera stereo observations

Cited by 84 publications

References 26 publications

The role of substrate characteristics in producing anomalously young crater retention ages in volcanic deposits on the Moon: Morphology, topography, subresolution roughness, and mode of emplacement of the Sosigenes lunar irregular mare patch

The role of substrate characteristics in producing anomalously young crater retention ages in volcanic deposits on the Moon: Morphology, topography, subresolution roughness, and mode of emplacement of the Sosigenes lunar irregular mare patch

Geological mapping and chronology of lunar landing sites: Apollo 11

The Cauchy 5 Small, Low‐Volume Lunar Shield Volcano: Evidence for Volatile Exsolution‐Eruption Patterns and Type 1/Type 2 Hybrid Irregular Mare Patch Formation

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