DFT study of the reduction reaction of calcium perchlorate on olivine surface: Implications to formation of Martian’s regolith

Escamilla‐Roa, Elizabeth; Zorzano, María Paz; Martín‐Torres, Javier; Hernández-Laguna, Alfonso; Sainz‐Díaz, C. Ignacio

doi:10.1016/j.apsusc.2020.145634

Cited by 8 publications

(2 citation statements)

References 66 publications

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“…The interface reaction between olivine and acidic solutions is related to the sustainable development in the fields ranging from the Earth and other celestial bodies’ crust evolution − to the carbon dioxide removal from the atmosphere . The dissolution rates of olivine minerals can help us understand the processes of rock metamorphism, revealing the dynamics of geological evolution .…”

Section: Introductionmentioning

confidence: 99%

Discontinuous Dissolution Mechanism of Olivine Deduced from a Topography Observation Method

Li,

Pedrosa,

Wang

et al. 2023

Langmuir

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Section: Introductionmentioning

confidence: 99%

Discontinuous Dissolution Mechanism of Olivine Deduced from a Topography Observation Method

Li,

Pedrosa,

Wang

et al. 2023

Langmuir

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“…Regarding the occurrence of calcium and magnesium perchlorate (Mg(ClO 4 ) 2 ) on Mars, the recent detections in the loose top regolith suggests a global occurrence, that is expected by wind mixing. Evaluating the formation conditions, calcium perchlorate might be produced by UV irradiance under Martian conditions with olivine minerals (Escamilla-Roa et al, 2020), while atmospheric origin is also proposed (Catling et al, 2010) -both models favour nearly global formation. If this salt have been produced by evaporation, it might show specific surface occurrence, however since there are no such observations the best current estimation is to consider a globally homogeneous presence with moderately small concentration (below 1%).…”

Section: Introductionmentioning

confidence: 99%

Deliquescence probability maps of Mars and key limiting factors using GCM model calculations

Pál,

Kereszturi

2021

Preprint

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There may be a chance of small-scale ephemeral liquid water formation on present day Mars, even though the current climate does not support the existence of larger bodies of water. Through a process called deliquescence, hygroscopic salts can enter solution by absorbing water vapor directly from the atmosphere. Due to the absence of in-situ deliquescence experiments so far, the most reliable way to forecast deliquescence is through atmospherical modeling, however, the locations and times when salty liquid water could emerge are not yet well known. In this paper we present our results of likely brine formation on Mars, their proposed locations and seasons, as well as the possible limiting factors. For our calculations we used the data of Laboratoire de Météorologie Dynamique Mars General Circulation Model version 5. The results show that from L s 35 • -L s 160 • , between 9 PM and 11 PM there is a good chance for calcium perchlorate deliquescence above 30 • N, while in this zone the ideal regions are concentrated mostly to Acidalia Planitia and Utopia Planitia between 1 AM and 3 AM. We found that in the Southern Hemisphere, between L s 195 • and L s 320 • , there is a noticeable, but weaker band in the vicinity of 60 • S, and both Argyre Planitia and Hellas Planitia show some chance for brine formation. According to our statistics the key limiting factor of deliquescence could be relative humidity in most cases. Our results suggest that during summer -early fall seasons, there could be deliquescence in both hemispheres in specific areas from the late evening until the early morning hours. There are only few studies detailing the geological and temporal distribution of brine formation through deliquescence, thus this work could be used as a good guide for future landing site analysis or in choosing a specific location for further research.

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Multiscale investigation of olivine (0 1 0) face dissolution from a surface control perspective

Wang

Shen

et al. 2021

Applied Surface Science

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DFT study of the reduction reaction of calcium perchlorate on olivine surface: Implications to formation of Martian’s regolith

Cited by 8 publications

References 66 publications

Discontinuous Dissolution Mechanism of Olivine Deduced from a Topography Observation Method

Discontinuous Dissolution Mechanism of Olivine Deduced from a Topography Observation Method

Deliquescence probability maps of Mars and key limiting factors using GCM model calculations

Multiscale investigation of olivine (0 1 0) face dissolution from a surface control perspective

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