A stratigraphic study of southern Oceanus Procellarum using Clementine multispectral data

Heather, D.; Dunkin, S. K.

doi:10.1016/s0032-0633(02)00124-1

Cited by 32 publications

(38 citation statements)

References 6 publications

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“…In these cases, wrinkle ridges form from contractional deformation of the volcanic plains, and where there is subsurface topography, such as a flooded impact crater, the topography can act as a stress concentrator that localizes deformation of the near-surface material. In the case of the Letrone-Flamsteed region of southern Oceanus Procellarum on the Moon, the crater Letrone is embayed and modified, with its northern margin completely flooded (Whitford-Stark and Mustard and Head, 1996), while farther to the north, the crater Flamsteed is almost completely buried by mare basalts (Pieters et al, 1980;Heather and Dunkin, 2002), forming an incipient wrinkle-ridge ring as part of the regional northwest-southeast-trending system in Oceanus Procellarum . The presence of wrinkle-ridge rings is generally interpreted to imply flooding of a crater to a level above its rim crest and subsequent deformation of the plains.…”

Section: Additional Criteria For Recognition Of Volcanic Plains: Sequmentioning

confidence: 99%

Volcanism on Mercury: Evidence from the first MESSENGER flyby for extrusive and explosive activity and the volcanic origin of plains

Head

Murchie

Prockter

et al. 2009

Earth and Planetary Science Letters

118

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Section: Additional Criteria For Recognition Of Volcanic Plains: Sequmentioning

confidence: 99%

Volcanism on Mercury: Evidence from the first MESSENGER flyby for extrusive and explosive activity and the volcanic origin of plains

Head

Murchie

Prockter

et al. 2009

Earth and Planetary Science Letters

118

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“…The entire Marius Hills plateau stretches a little further south than this, to approximately 6.00°N. This part of the plateau had already been incorporated into another region as part of a separate study [ Heather , 2000; Heather and Dunkin , 2002] and mosaicked at a resolution of 200 m/pixel. For all studies a series of Clementine images were produced, including multispectral ratio, FeO, and TiO 2 maps.…”

Section: Data Reductionmentioning

confidence: 99%

“…These values were then tested successfully via independent mapping of the Flamsteed region of Oceanus Procellarum, previously mapped telescopically by Pieters et al [1980]. Full details of this validation and the mapping technique employed in this study is given by Heather [2000], and it has been applied to Oceanus Procellarum on a more regional scale by Heather and Dunkin [2002].…”

Section: Spectral Mapping Of the Mare Basalts In Marius Hillsmentioning

confidence: 99%

“…Marius Basalt 1 represents the member that was spectrally characterized in the Flamsteed region by Pieters et al [1980] and was largely fed by the 210 km long rille on the southwestern edge of the Marius Hills plateau [ Whitford‐Stark and Head , 1980], visible in the m5 unit in Figure 2. This unit extends from the plateau to cover a large portion of Oceanus Procellarum to the south and southwest [ Whitford‐Stark and Head , 1980; Heather and Dunkin , 2002].…”

Section: Spectral Mapping Of the Mare Basalts In Marius Hillsmentioning

confidence: 99%

“…The actual volume erupted will be much greater since extensive flows sourced from Marius Hills can be found outside the region mapped here. Details of how the values on the Marius Hills plateau combine with those for the rest of Oceanus Procellarum are provided by Heather [2000] and Heather and Dunkin [2002].…”

Section: Spectral Mapping Of the Mare Basalts In Marius Hillsmentioning

confidence: 99%

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Volcanism on the Marius Hills plateau: Observational analyses using Clementine multispectral data

2003

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We have studied the Marius Hills region and mapped the spectrally distinct flows present for the first time, using photographic and Clementine multispectral data. The basalts on the plateau are varied in age and composition but are dominated by a high‐titanium Eratosthenian basalt, most likely from the same source as the Flamsteed Basalt, further south. The thickness of the basalts across the plateau is consistently greater than 120 m and is considerably thicker in some areas. A lower limit of 5320 km3 of basalts has been erupted onto the plateau. The domes and cones in the region do not appear to be related to any specific basalt or volcanic episode but occur at all levels in the stratigraphy that can be derived in the region. The eruption conditions required to form these constructs indicate that they must represent a series of separate volcanic episodes occurring throughout the history of the plateau. Cones on the Marius plateau are dominated by a strong glassy signature and often have an associated microlitic structure. Examples are shown of localized microlitic or glassy materials in regions where no cone is evident in the photographic data. These features are proposed to represent short‐lived pyroclastic episodes that have deposited glassy and microlitic units on the plateau but have not been maintained for long enough to develop a cone. The volcanic history of the Marius Hills region is extremely complex, and most likely involved several separate episodes of volcanism with a large contrast in eruption styles and characteristics.

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Characterization of melt and ejecta deposits of Kepler crater from remote sensing data

2014

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We used Moon Mineralogy Mapper (M3), Arecibo and Mini‐RF radar, and Diviner radiometer data with Lunar Reconnaissance Orbiter (LRO) Camera and Kaguya Terrain Camera images to characterize the target, ejecta, and impact melt‐rich lithologies in and around lunar central peak crater Kepler. M3 data indicate the impact melt rocks of crater floor to be high‐Ca pyroxene dominated, distinct from the low‐Ca pyroxene‐dominated crater wall. The central uplift is high‐Ca pyroxene dominated, and has higher albedo. These observations are consistent with thin mare basalts underlain by noritic Imbrium ejecta, underlain by gabbroic crustal material. M3 data reveal an enigmatic, splash‐like feature of melt‐rich material on the southeastern (uprange) crater wall and flank. M3 data also highlight halos around Kepler. In detail the halos are slightly variable, but in broad terms they define a consistent feature, offset to the inferred downrange direction, and interpreted to reflect the distribution of glass‐bearing impact breccia. The radar data sets show most of the proximal ejecta to be radar‐bright. However, Diviner rock abundance data do not indicate the presence of blocks on the surface nor can they be seen using LRO Narrow Angle Camera images. Thus, the blocks giving rise to the enhanced radar signal are buried. Beyond the radar‐bright zone, a subtle radar‐dark halo emerges, coincident with a region of very low rock abundance in Diviner data. This multidisciplinary approach provides a robust analysis of the main characteristics of a lunar complex crater and reveals previously unidentified features related to the distribution of impact melt.

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A stratigraphic study of southern Oceanus Procellarum using Clementine multispectral data

Cited by 32 publications

References 6 publications

Volcanism on Mercury: Evidence from the first MESSENGER flyby for extrusive and explosive activity and the volcanic origin of plains

Volcanism on Mercury: Evidence from the first MESSENGER flyby for extrusive and explosive activity and the volcanic origin of plains

Volcanism on the Marius Hills plateau: Observational analyses using Clementine multispectral data

Characterization of melt and ejecta deposits of Kepler crater from remote sensing data

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