The lunar Gruithuisen silicic extrusive domes: Topographic configuration, morphology, ages, and internal structure

Иванов, М. А.; Head, J. W.; Bystrov, A.

doi:10.1016/j.icarus.2015.12.015

Cited by 33 publications

(52 citation statements)

References 58 publications

(75 reference statements)

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“…A geologic map (Figure ) was produced, and we interpret the geological evolutionary history of the Rümker region as follows: The Imbrium impact at 3.92 Ga ago generated a complex multiring system (Snape et al, ) and the outer ring materials formed the Ith unit in the area (Scott & Eggleton, ; Spudis et al, ). Ejecta of the Iridum impact (3.84–3.7 Ga; Wagner et al, ) formed the lineated terrain in the north of Mons Rümker before 3.71 Ga (Zhao et al, ). The earliest detectable basaltic volcanism in the area erupted around 3.72 Ga ago (Hiesinger et al, ), forming medium to high‐titanium mare basalts belonging to the Repsold Formation (Whitford‐Stark & Head, ). Basaltic volcanism was active from 3.71 to 3.51 Ga ago in Mons Rümker, forming plateau basalts IR1 (3.71 Ga), IR2 (3.58 Ga), and IR3 (3.51 Ga; Zhao et al, ). Silica‐rich domes (Idm) formed contemporaneously to, or a little earlier than, Mons Rümker by silica/felsite volcanic activity (Glotch et al, , ; Head & McCord, ; Head & Wilson, ; Ivanov et al, ; Wilson & Head, ). The major phase of basaltic volcanism occurred during the Late Imbrian Period, forming very low‐Ti to low‐Ti mare basalts (Im1, 3.42 Ga; Im2, 3.39 Ga; Im3, 3.16 Ga). NW‐oriented wrinkle ridges in Oceanus Procellarum were tectonically generated around 3.35 Ga ago (Yue et al, ). The youngest phase of mare volcanism started at ~2.30 Ga ago and ceased at ~1.21 Ga ago, forming four episodes of mare units (Em1, 2.30 Ga; Em2, 2.13 Ga; Em3, 1.51 Ga; Em4, 1.21 Ga). The youngest mare volcanism (with elevated titanium content) formed the Em4 unit. …”

Section: Discussionmentioning

confidence: 99%

Geology and Scientific Significance of the Rümker Region in Northern Oceanus Procellarum: China's Chang'E‐5 Landing Region

et al. 2018

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The Rümker region (41–45°N, 49–69°W) is located in northern Oceanus Procellarum of the Moon. Mons Rümker is the most distinctive geological feature in the area. The region is characterized by prolonged lunar volcanism (Late Imbrian Period to Eratosthenian Period), forming multiple geologic units in the area, including very low‐Ti to low‐Ti mare basalts, high‐Ti mare basalts, and volcanic complexes. Each geologic unit has distinct element composition and mineral assemblages. The Rümker region, overlying the Procellarum KREEP Terrain, was selected as the landing region for China's Chang'E‐5 lunar sample return mission. Prelanding analyses of the geologic context and scientific potential are reported in this contribution. We conducted detailed geological mapping using image, spectral, and altimetry data. Fourteen geological units were defined, a geologic map was constructed, and the geologic history was outlined. The western mare units (Im1, Im2, and Im3) are Imbrian‐aged (~3.4–3.5 Ga) representing the major stage of lunar mare eruptive volcanism. The eastern young mare units (Em3 and Em4; <2 Ga) are among the youngest mare basalts on the Moon. They have never been explored in situ or studied in the laboratory. We suggest that samples returned from the eastern mare unit (Em4) could answer many fundamental questions and that this unit should be listed as the top priority landing site for Chang'E‐5 sample return mission.

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Section: Discussionmentioning

confidence: 99%

Geology and Scientific Significance of the Rümker Region in Northern Oceanus Procellarum: China's Chang'E‐5 Landing Region

et al. 2018

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“…The very rare occurrence on the Moon of the morphologically and spectroscopically distinctive Gruithuisen (Figure 32a) and Mairan domes in northeast Oceanus Procellarum (Head and McCord, 1978;Glotch et al, 2011;Kusuma et al, 2012;Ivanov et al, 2015) and the farside domes between the craters Belkovich and Compton Chauhan et al, 2015) (Figure 32b) implies the localized eruption of unusually viscous,…”

Section: G Non-mare Volcanic Domes and Complexes: Relation To Basaltmentioning

confidence: 99%

“…Wilson and Head (2016a) showed that substantial volumes, (~5000 km 3 ) of basaltic magma could be emplaced as intrusions at or near the base of the crust under suitable circumstances. The silicic domes are inferred to have been formed ~3.8 Ga ago (Wagner et al, 2002(Wagner et al, , 2010Ivanov et al, 2015) concurrently with early mare history (Figure 1c), and at a time when the lithosphere was relatively thin (Figures 2, 15), and buoyant mantle plumes were more likely to pond at or near the base of the crust. The volumes of the larger domes are ~300-500 km 3 (Wilson and Head, 2003b), an order of magnitude smaller than a possible 5000 km 3 basalt intrusion, and so partial melting of overlying crust and fractional crystallization of sill magma are both viable sources of the silicic melt on thermal grounds .…”

Section: G Non-mare Volcanic Domes and Complexes: Relation To Basaltmentioning

confidence: 99%

“…Using these combined data,Jolliff et al (2011) interpreted these features as volcanic domes formed from viscous lava enriched in silica or alkaliCompton-Belkovich thorium anomaly as a rare occurrence of non-basaltic volcanism on the lunar farside in an area far removed from the Procellarum-KREEP terrain. In contrast to the pre-mare or syn-early mare ages of the Gruithuisen domes(Wagner et al, 2002;Ivanov et al, 2015),Jolliff et al (2011) interpreted the ComptonBelkovich feature to be Copernican in age on the basis of the sparse number of superposed craters observed on the feature and deposit, and preservation of the small dome features. A maximum age of Lower Imbrian is established from its superposition on the Lower Imbrian-aged Compton crater.…”

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confidence: 99%

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Generation, ascent and eruption of magma on the Moon: New insights into source depths, magma supply, intrusions and effusive/explosive eruptions (Part 2: Predicted emplacement processes and observations)

Head

Wilson

2017

Icarus

186

197

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1 Highlights  Mare basalt eruption process predictions are compared to observed features/deposits.  Single dike event magma volume predicted to be 10 2 -10 3 km 3 ; dikes 40-100 m by 60-100 km. Shallower-source dikes continuous from source to surface; deeper dikes detach from source. Dikes reaching surface form wide range of predicted/observed effusive/explosive eruption types. Intrusion is favored in thicker farside crust; extrusion is favored on thin nearside crust. AbstractWe utilize a theoretical analysis of the generation, ascent, intrusion and eruption of basaltic magma on the Moon to develop new insights into magma source depths, supply processes, transport and emplacement mechanisms via dike intrusions, and effusive and explosive eruptions. We make predictions about the intrusion and eruption processes and compare these with the range of observed styles of mare volcanism, and related features and deposits. Density contrasts between the bulk mantle and regions with a greater abundance of heat sources will cause larger heated regions to rise as buoyant melt-rich diapirs that generate partial melts that can undergo collection into magma source regions; diapirs rise to the base of the anorthositic crustal density trap (when the crust is thicker than the elastic lithosphere) or, later in history, to the base of the lithospheric rheological trap (when the thickening lithosphere exceeds the thickness of the crust). Residual diapiric buoyancy, and continued production and arrival of diapiric material, enhances melt volume and overpressurizes the source regions, producing sufficient stress to cause brittle deformation of the elastic part of the overlying lithosphere; a magma-filled crack initiates and propagates toward the surface as a convex upward, blade-shaped dike. The volume of magma released in a single event is likely to lie in the range 10 2 km 3 to 10 3 km 3 , corresponding to dikes with widths of 40-100 m and both vertical and horizontal extents of 60-100 km, favoring eruption on the lunar nearside. Shallower magma sources produce dikes that are continuous from the source region to the surface, but deeper sources will propagate dikes that detach from the source region and ascend as discrete penny-shaped structures. As the Moon cools with time, the lithosphere thickens, source regions become less abundant, and rheological traps become increasingly deep; the state of stress in the lithosphere becomes increasingly contractional, inhibiting dike emplacement and surface eruptions.In contrast to small dike volumes and low propagation velocities in terrestrial environments, lunar dike propagation velocities are typically sufficiently high that shallow sill formation is not favored; local low-density breccia zones beneath impact crater floors, however, may cause lateral magma migration to form laccoliths (e.g., Vitello Crater) and sills (e.g., Humboldt Crater) in floor-fractured craters. Dikes emplaced into the shallow crust may stall and produce crater chains due to active andpassive gas venting (e.g., Men...

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“…using the standard ArcGIS tool) that cover all areas of interest. Implementation of these tools allows processing of large volumes of data for morphometric and geologic analysis of planetary surface (Ivanov et al, 2016). …”

Section: Volume Measurementmentioning

confidence: 99%

Automation of Morphometric Measurements for Planetary Surface Analysis and Cartography

Kokhanov¹,

Bystrov²,

Kreslavsky³

et al. 2016

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

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ABSTRACT:For automation of measurements of morphometric parameters of surface relief various tools were developed and integrated into GIS. We have created a tool, which calculates statistical characteristics of the surface: interquartile range of heights, and slopes, as well as second derivatives of height fields as measures of topographic roughness. Other tools were created for morphological studies of craters. One of them allows automatic placing of topographic profiles through the geometric center of a crater. Another tool was developed for calculation of small crater depths and shape estimation, using C++ programming language. Additionally, we have prepared tool for calculating volumes of relief features from DTM rasters. The created software modules and models will be available in a new developed web-GIS system, operating in distributed cloud environment.

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The lunar Gruithuisen silicic extrusive domes: Topographic configuration, morphology, ages, and internal structure

Cited by 33 publications

References 58 publications

Geology and Scientific Significance of the Rümker Region in Northern Oceanus Procellarum: China's Chang'E‐5 Landing Region

Geology and Scientific Significance of the Rümker Region in Northern Oceanus Procellarum: China's Chang'E‐5 Landing Region

Generation, ascent and eruption of magma on the Moon: New insights into source depths, magma supply, intrusions and effusive/explosive eruptions (Part 2: Predicted emplacement processes and observations)

Automation of Morphometric Measurements for Planetary Surface Analysis and Cartography

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