Shallow subsurface basalt layer along Cerberus Fossae, Mars: Insights from SHARAD, HiRISE, and CRISM analysis

Harish,; Kimi, K.B.; Tuhi, S.; Baliyan, S.; Mangold, N.; El‐Maarry, M. R.; Vijayan, S.

doi:10.1016/j.icarus.2022.115343

Cited by 1 publication

(5 citation statements)

References 44 publications

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“…(2021) and Harish et al. (2023) discussing the material properties in Elysium Planitia analyzed by SHARAD. Xiong et al.…”

Section: Discussionmentioning

confidence: 99%

“…Harish et al. (2023) followed a similar approach based on HiRISE DTMs of visible layering exposed along Cerberus Fossae, finding three main units: a 3–5 m thick regolith cover, a ∼30 m thick layered unit, and ∼260 m thick bouldery unit. They hypothesized that the stratigraphic boundary between the second and the third unit at ∼34 m depth corresponds to a dielectric interface capable of generating reflectors detected in SHARAD profiles across Cerberus Fossae, estimating a bulk real permittivity of 9.34 ± 1.01 (at 1 σ ), in turn suggesting the presence of thick, dense shergottite‐type basaltic material along the Cerberus Fossae.…”

Section: Discussionmentioning

confidence: 99%

“…Harish et al. (2023) also calculated the loss tangent of the same materials following the methods of Campbell et al. (2008), obtaining a mean loss tangent of 0.027 ± 0.01, which is at least an order of magnitude higher than that of water ice found elsewhere on Mars (e.g., Petersen et al., 2018) and is compatible with basaltic lava flows (e.g., Morgan et al., 2015).…”

Section: Discussionmentioning

confidence: 99%

“…There have been two recent papers by Xiong et al (2021) and Harish et al (2023) discussing the material properties in Elysium Planitia analyzed by SHARAD. Xiong et al (2021) used HiRISE DTMs of impact crater terraces in Elysium Planitia to identify possible subsurface interfaces that may correspond to SHARAD reflectors and derive the bulk real permittivity, which they estimated to be 3.12, suggesting the possible presence of subsurface water ice.…”

Section: The Role Of Lava Versus Icementioning

confidence: 99%

“…They hypothesized that the stratigraphic boundary between the second and the third unit at ∼34 m depth corresponds to a dielectric interface capable of generating reflectors detected in SHARAD profiles across Cerberus Fossae, estimating a bulk real permittivity of 9.34 ± 1.01 (at 1σ), in turn suggesting the presence of thick, dense shergottite-type basaltic material along the Cerberus Fossae. Harish et al (2023) also calculated the loss tangent of the same materials following the methods of Campbell et al (2008), obtaining a mean loss tangent of 0.027 ± 0.01, which is at least an order of magnitude higher than that of water ice found elsewhere on Mars (e.g., Petersen et al, 2018) and is compatible with basaltic lava flows (e.g., Morgan et al, 2015).…”

Section: The Role Of Lava Versus Icementioning

confidence: 99%

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Revealing Elysium Planitia's Young Geologic History: Constraints on Lava Emplacement, Areas, and Volumes

Voigt,

Hamilton,

Steinbrügge

et al. 2023

JGR Planets

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Elysium Planitia includes several outflow channels that were likely carved by aqueous erosion and subsequently infilled by younger lava flows, making Elysium Planitia the youngest volcanic terrain on Mars. Studying this region is critical for constraining the recent hydrological and thermal evolution of the planet. Here, we investigate the lava flow areas, thicknesses, and volumes in Elysium Planitia using Context (CTX) camera images in combination with SHAllow RADar (SHARAD) sounder data. Compiling 1,777 reflectors over an area of 9,126,790 km2 allows us to reconstruct the subsurface landscape evolution over time. Our findings show that Elysium Planitia is composed of material from about 40 episodes of effusive volcanic activity. We report volumes for individual eruptions of 4,000 ± 1,600 km3 infilling Athabasca Valles, 12,200 ± 2,500 km3 in Marte Vallis, and 16,000 ± 4,000 km3 in Rahway Valles for the major flow units and volumes as small as 100 ± 50 km3 in Cerberus Plains. The surface morphologies and inferred dielectric properties of lobe interfaces suggests that the regions consists of basaltic lava. The region also experienced multiple aqueous flooding events. Although, we found evidence of past lava–water interactions, present‐day ground‐ice (if present) is likely limited to local patches. Further, the pre‐eruption landscape reveals that the aqueously carved Marte Vallis is more areal extensive, but shallower than previously suggested, with a likely paleo‐flow direction from northwest to southeast. The channel is most likely sourced from a segment in the northwestern portion of Cerberus Fossae, and is now buried by multiple Late Amazonian lavas with the same lava flow direction.

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“…(2021) and Harish et al. (2023) discussing the material properties in Elysium Planitia analyzed by SHARAD. Xiong et al.…”

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%