Investigating the volcanic versus aqueous origin of the surficial deposits in Eastern Elysium Planitia, Mars

Voigt, Joana; Hamilton, C. W.

doi:10.1016/j.icarus.2018.03.009

Cited by 30 publications

(41 citation statements)

References 60 publications

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“…The surrounding areas have a higher topography and their surface units are interpreted to be older. To the south, there is a Cerberus Fossae 1 (AEc 1 ) unit, which is interpreted to be a part of the Medusae Fossae unit (Voigt & Hamilton, 2018). To the north, it is mainly composed of the Noachian‐age Nepenthes Mensae unit.…”

Section: Methodsmentioning

confidence: 99%

“…The sources of the two channels is indicated by a red star shown in Figure 1. Marte Vallis is inferred to be formed during the Amazonian Period, and its age is ≤200 Ma (Voigt & Hamilton, 2018). The source of floodwater that carved Marte Vallis may have originated from an eastern fissure of Cerberus Fossae, which has since been buried by lava flows and is 180 km southeast to the visible southeast end of the fissure and the channel depth which was estimated to be at least 80 m based on SHARAD data (Morgan et al., 2013).…”

Section: Methodsmentioning

confidence: 99%

“…Voigt and Hamilton (2018) mapped 19 morphologically distinct regions using facies over the eastern Elysium Planitia, including Eastern Cerberus Fossae, Rahway Valles and Marte Vallis, showing this region was resurfaced by at least two volcanic flows with much younger ages of 20 and 8.8 Ma, as there is an erosional unconformity located between two youngest lava flow units in Marte Vallis. They infer that the outflow channels were carved out by catastrophic fluvial events and emplaced by more recent flood lava (Voigt & Hamilton, 2018). From several threads of clues, there appears to be a consensus that aqueous floods had carved the outflow channels which were later emplaced by lava flows (Keszthelyi et al., 2017; G. A. Morgan et al., 2013).…”

Section: Introductionmentioning

confidence: 99%

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Subsurface Reflectors Detected by SHARAD Reveal Stratigraphy and Buried Channels Over Central Elysium Planitia, Mars

Xiong

Tao

Persaud

et al. 2021

Earth and Space Science

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The interior morphology of Cerberus Fossae consists of a steep, layered upper slope and a gentler lower slope, which are presumably composed of exposed bedrock and talus, respectively (Plescia, 2003). Various landforms observed in this region have resulted in several hypotheses as to the origin of the Cerberus plains material, from a purely aqueous origin to a purely volcanic one. For example, Athabasca Valles is thought to have been carved by a high-discharge flood of water based on streamlined islands, notches on the sides of the breach hanging valleys and a low number of tributaries, while other authors have argued that this channel might be carved by fluid lava, which is supported by fissure vents (

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Subsurface Reflectors Detected by SHARAD Reveal Stratigraphy and Buried Channels Over Central Elysium Planitia, Mars

Xiong

Tao

Persaud

et al. 2021

Earth and Space Science

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“…Lava flow features have been attributed to inflation on a wide range of planetary bodies, including Mars (e.g., Bleacher et al, 2017; Crown & Ramsey, 2017; Giacomini et al, 2009; Glaze et al, 2003; Hamilton et al, 2010, 2018; Keszthelyi et al, 2000, 2008; Mouginis‐Mark & Yoshioka, 1998; Voigt & Hamilton, 2018), Venus (Roberts et al, 1992), and the Moon Garry et al, 2012). However, the origins of these landforms are debated—particularly on Mars where lobate flow units have also been interpreted as the products of viscous mudflows (e.g., Christiansen, 1989; De Hon et al, 1999; Morris & Mouginis‐Mark, 2006; Pedersen, 2013; Pedersen & Head, 2010; Wilson & Mouginis‐Mark, 2003, 2014).…”

Section: Discussion: Implications For Identifying Inflation Features mentioning

confidence: 99%

Lava‐Rise Plateaus and Inflation Pits in the McCartys Lava Flow Field, New Mexico: An Analog for Pāhoehoe‐Like Lava Flows on Planetary Surfaces

et al. 2020

Self Cite

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Basaltic lava flows are common on the surface of the Earth and other terrestrial bodies. However, inflation—including a combination of initially rapid molten core thickening and gradual crustal growth—must be accounted for to enable accurate reconstructions of eruption parameters from observed lava flow morphologies. The shape of an inflated lava flow can change significantly over time. Therefore, incorrectly attributing the flow's final thickness to its dimensions in an initially fully molten state will yield excessively high flow rates, erroneous rheological properties, and unreasonably short eruption durations. To develop improved criteria for identifying inflated lava flows, we examined the McCartys lava flow field in New Mexico, USA. This locality provides an example of how pāhoehoe‐like lava lobes can coalesce and coinflate to form interconnected lava‐rise plateaus with internal inflation pits. These structures were examined using a combination of field observations, low‐altitude kite‐based imaging, and quantitative geomorphology using high‐resolution (1.47 cm/pixel) orthomosaics and stereo‐derived digital terrain models. These observations were used to identify characteristics and diagnostics of inflation, thereby facilitating the interpretation of comparable landforms on other planetary surfaces. Lava‐cooling models were also used to estimate the lava emplacement duration of the ~20‐m‐thick flows by demonstrating that the ~8‐m‐thick upper crust exposed within inflation clefts in the southern part of the McCartys lava flow field would have required 1.2–2.5 years of continuous lava supply to form. This places a minimum bound on the total eruption duration, and implies that comparably thick inflated flows on Mars required years to form.

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“…, aeolian ridges (Berman et al, 2018;Chojnacki et al, 2014Chojnacki et al, , 2017, and fluvial deposits (Voigt and Hamilton, 2018;Tirsch et al, 2018;Adler et al, 2019;Davis et al, 2018;Hamilton et al, 2018;Stack et al, 2016;Wilson et al, 2018). DEMs also fulfil a critical mission requirement when searching for potential rover landing-sites (Stack et al, 2016;Golombek et al, 2017Golombek et al, , 2012Grant et al, 2018).…”

mentioning

confidence: 99%

Creating HiRISE digital elevation models for Mars using the open-source Ames Stereo Pipeline

Hepburn¹,

Holt²,

Hubbard³

et al. 2019

Preprint

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Abstract. The present availability of sub-decametre digital elevation models on Mars – crucial for the study of surface processes – is scarce. In contrast to the globally-available but low-resolution datasets, such models enable the study of landforms 3000 stereo pairs at 25 cm/pixel resolution, enabling the creation of high-resolution digital elevation models (1–2 m/pixel). However, only ~ 500 of these pairs have been processed and made publicly available to date. Existing pipelines for the production of digital elevation models from stereo-pairs, however, are built upon commercial software, rely upon sparsely-available intermediate data, or are reliant on proprietary algorithms. Here, we present and test the output of a new pipeline for producing digital elevation models from HiRISE stereo pairs that is built entirely upon the open source NASA Ames Stereo Pipeline photogrammetric software, making use of freely available data for cartographic rectification. This pipeline is implemented here on a research computing cluster, but can also be used on consumer-grade UNIX computers. The four output digital elevation models produced using the pipeline presented here are globally well-registered, with accuracy similar to those of multiple digital elevation models produced elsewhere.

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Investigating the volcanic versus aqueous origin of the surficial deposits in Eastern Elysium Planitia, Mars

Cited by 30 publications

References 60 publications

Subsurface Reflectors Detected by SHARAD Reveal Stratigraphy and Buried Channels Over Central Elysium Planitia, Mars

Subsurface Reflectors Detected by SHARAD Reveal Stratigraphy and Buried Channels Over Central Elysium Planitia, Mars

Lava‐Rise Plateaus and Inflation Pits in the McCartys Lava Flow Field, New Mexico: An Analog for Pāhoehoe‐Like Lava Flows on Planetary Surfaces

Creating HiRISE digital elevation models for Mars using the open-source Ames Stereo Pipeline

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