Geology, in-situ resource-identification and engineering analysis of the Vernal crater area (Arabia Terra): A suitable Mars human landing site candidate

Development of Martian saline seep models and their implications for planetary protection

“…However, the presence of B. subtilis and additional Bacillus spore-formers provide potential forward contamination routes. Further, the lower temperature limit for H. titanicae is 4 C for consistent growth which is within the known Martian temperature range [ 10 , 11 , 70 , 71 ]. H. titanicae resistance to UV radiation is unknown, however, the biofilm morphology can exhibit greater tolerance to UV radiation and other environmental stresses than individual cells of the same species [ 72 ].…”

“…We used a simple, proof-of-concept experiment design to eliminate confounding factors such as the influence of substratum on biofilm formation that would occur using a more complicated regolith simulant. The model was kept at room temperature as temperatures up to 22 °C are found on the surface of Mars during a summer sol [ 10 , 11 ]. The high-carbon experiment was designed as a baseline for model development to compare several aspects that are strong drivers of microbial growth without being carbon-limited to confirm biofilm formation.…”

“…Like Earth, Mars is highly heterogenous with varying temperatures, topography, and soil composition throughout the planet. The temperatures on the surface of Mars average −63 °C compared to Earth’s average of 13 °C [ 9 ], although mathematical temperature modeling predicts surface temperatures in the lower latitudes can approach 22 °C during a sunny summer sol [ 10 , 11 ]. Water in the form of ice exists in many places on Mars, but negligible concentrations are present as water vapor in the atmosphere [ 12 ].…”

Protracted Hydrogeological Activity in Arabia Terra, Mars: Evidence From the Structure and Mineralogy of the Layered Deposits of Becquerel Crater

“…As discussed, non-radial outward dips are not agreeable with the katabatic winds model (Kite et al, 2013) and the off center location of the ELD Mound makes an airfall deposition problematic. If layers were formed by aeolian deposition, deposit remnants should be found elsewhere around the crater as other craters in Arabia Terra have been described (Annex & Lewis, 2020;Murana, 2018;Pajola et al, 2022;Pondrelli et al, 2019;Schmidt et al, 2021), not localized to a specific location. Likewise, aeolian dust collected onto seasonal ice (Michalski & Niles, 2012) could produce thinning and thickening sequences (Lewis & Aharonson, 2014), however the lack of glacial or periglacial morphology in the study area means that ice likely did not play a major role in the deposition.…”

Groundwater‐Controlled Deposition of Equatorial Layered Deposits in Central Arabia Terra, Mars

“…Proposed formational hypotheses include groundwater moderated aeolian loess (Andrews‐Hanna & Lewis, 2011; Andrews‐Hanna et al., 2007, 2010; Annex & Lewis, 2020; Bridges & Muhs, 2012; Cadieux & Kah. 2015; Grotzinger et al., 2005; Kite, Halevy, et al., 2013; Kite, Lewis, et al., 2013; Murchie, Roach, et al., 2009; Zabrusky et al., 2012) or pyroclastic deposits (Hynek et al., 2002; Kerber et al., 2012; Scott & Tanaka, 1982); groundwater‐fed evaporitic playa deposits (Andrews‐Hanna & Lewis, 2011; Andrews‐Hanna et al., 2007; Zabrusky et al., 2012), spring deposits or mud volcanoes deposits (Franchi et al., 2014; Pajola et al., 2022; Pondrelli et al., 2011, 2015, 2019; Rossi et al., 2008); lacustrine deposits (Fueten et al., 2017; Lucchitta et al., 1992; Mangold et al., 2020; Newsom et al., 2003; Salese, Kleinhans, et al., 2020); ground ice melt‐driven cemented deposits (Cadieux & Kah, 2015; Niles & Michalski, 2009); sub‐ice volcanic flow deposits (Chapman & Tanaka, 2002; Komatsu et al., 2004); weathered basalts (Madden et al., 2004); other mixed‐aeolian deposits (Day & Catling, 2020; Michalski & Niles, 2012; Tanaka, 2000); impact base surge deposits (Knauth et al., 2005).…”