Reflectance study of ice and Mars soil simulant associations – I. H2O ice

Yoldi, Z.; Pommerol, Antoine; Poch, Olivier; Thomas, N.

doi:10.1016/j.icarus.2020.114169

Cited by 9 publications

(29 citation statements)

References 65 publications

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“…2) Yoldi et al [48] and [49] experimented on real water-ice samples of two different particle sizes (i) SPIPA-A (4.5±2.5µm) and (ii) SPIPA-B (67±31µm), and their intimate mixtures with two primary regolith -(i) JSC Mars-1 (24µm) and (ii) Dark Basalt (50wt% of the particles > 109µm and 50% < 109µm). Out of the above four samples they used three combinations at different proportions as described in Table 3.…”

Section: Discussionmentioning

confidence: 99%

“…Fig. 7: Calculated reflectance using Eq.5 has been plotted against measured reflectance values for the three sets of intimate mixtures in [49]. Data were derived from Fig.…”

Section: Discussionmentioning

confidence: 99%

“…Many experimental and theoretical modeling works have been conducted in the field of reflectance spectroscopy of intimate mixtures. Among them, [48], [49], [7], [8], [14], [15], [16], [17], [18], [26], [33], [34], [45], [40], [20], [21], [22] are important.…”

Section: Introductionmentioning

confidence: 99%

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A photometric study of regolith intimate mixing with ice-like impurity

Deb¹,

Chakraborty

2022

Eur. Phys. J. Plus

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Surfaces of solid solar system objects are covered by layers of particulate materials called regolith originated from their surface bedrock. They preserve important information about surface geological processes. Often regolith is composed of more than one type of particle in terms of composition, maturity, size, etc. Experiments and theoretical works are being carried out to constrain the result of mixing and extract the abundance of compositional end-members from regolith spectra. In this work we have studied, photometric light scattering from simulated surfaces made of two different materials -one is highly bright quartz particles (average diameter 78.336 µm) and the other moderately bright sandstone particles (average diameter 253.757 µm). The samples were mixed with varying proportions and investigated at normal illumination conditions to avoid the shadowing effect. Said combinations may resemble ice mixed regolith on various solar system objects and therefore it is important for in situ observations. We find that the combinations show a linear trend in the corresponding reflectance data in terms of their mixing proportion and some interesting facts come out when compared to previous studies.

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Section: Discussionmentioning

confidence: 99%

“…Fig. 7: Calculated reflectance using Eq.5 has been plotted against measured reflectance values for the three sets of intimate mixtures in [49]. Data were derived from Fig.…”

Section: Discussionmentioning

confidence: 99%

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A photometric study of regolith intimate mixing with ice-like impurity

Deb¹,

Chakraborty

2022

Eur. Phys. J. Plus

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“…No in situ measurements of the seasonal CO2 frost layer have yet been collected due to technical challenges in having a spacecraft survive through the winter (ICE-SAG, 2019). Laboratory experiments have begun to look at CO2 frost/ice formation (e.g., Portyankina et al, 2019), as well as at how both H2O and CO2 sublimation may interact with granular materials (e.g., Chinnery et al, 2018;Herny et al, 2019;Kaufmann and Hagermann, 2017;Massé et al, 2016;Mc Keown et al, 2017;Pommerol et al, 2019;Portyankina et al, 2019;Raack et al, 2017;Sylvest et al, 2016;Yoldi et al, 2021). By necessity due to present lab capabilities, such experiments are small-scale and simplified in terms of the variables incorporated.…”

Section: Open Questions For Seasonal Frost/ice and Related Landformsmentioning

confidence: 99%

“…The surface pressure of the martian atmosphere is 2-3 orders of magnitude less than that of the Earth, and Pluto's atmosphere is another ~3 orders of magnitude lower, providing a large physical range for future modeling that applies to a full suite of planetary atmospheres in the Solar System and elsewhere. Laboratory studies of H2O and CO2 ice (e.g., Chinnery et al, 2018;Kaufmann and Hagermann, 2017;Pommerol et al, 2019;Portyankina et al, 2019;Yoldi et al, 2021), as well as how evolution of such materials is altered through interaction between the ices and dust, coupled with Mars ice and environment observations provides the current best route for formulating and calibrating models of these strange ices under extraterrestrial conditions. Even if not providing a direct analog, study of martian ices may also help ground truth models and demonstrate how to interpret spacecraft observations and connect them with terrestrial experiments involving exotic ices.…”

Section: Aeolian Surface Processes and Meteorological Dynamicsmentioning

confidence: 99%

Modern Mars' geomorphological activity, driven by wind, frost, and gravity

et al. 2021

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Extensive evidence of landform-scale martian geomorphic changes has been acquired in the last decade, and the number and range of examples of surface activity have increased as more high-resolution imagery has been acquired. Within the present-day Mars climate, wind and frost/ice are the dominant drivers, resulting in large avalanches of material down icy, rocky, or sandy slopes; sediment transport leading to many scales of aeolian bedforms and erosion; pits of various forms and patterned ground; and substrate material carved out from under subliming ice slabs. Due to the ability to collect correlated observations of surface activity and new landforms with relevant environmental conditions with spacecraft on or around Mars, studies of martian geomorphologic activity are uniquely positioned to directly test surface-atmosphere interaction and landform formation/evolution models outside of Earth. In this paper, we outline currently observed and interpreted surface activity occurring within the modern Mars environment, and tie this activity to wind, seasonal surface CO2 frost/ice, sublimation of subsurface water ice, and/or gravity drivers. Open questions regarding these processes are outlined, and then measurements needed for answering these questions are identified. In the final sections, we discuss how many of these martian processes and landforms may provide useful analogs for conditions and processes active on other planetary surfaces, with an emphasis on those that stretch the bounds of terrestrial-based models or that lack terrestrial analogs. In these ways, modern Mars presents a natural and powerful comparative planetology base case for studies of Solar System surface processes, beyond or instead of Earth.

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