Planetary and Space Science最新文献

{"title":"Chemical processes during collisions of meteoroids with the Moon","authors":"A.A. Berezhnoy ,&nbsp;G.V. Belov ,&nbsp;C. Wöhler","doi":"10.1016/j.pss.2024.105942","DOIUrl":"10.1016/j.pss.2024.105942","url":null,"abstract":"<div><p>A realistic model of physico-chemical processes during collisions between meteoroids and the Moon considering condensation of refractory elements in the form of minerals and variable adiabatic index during expansion of impact-produced clouds was developed. Quenched chemical composition of impact-produced cloud is estimated. In accordance with this model relative fraction of atoms delivered to the lunar exosphere by impacts of meteoroids is significantly higher than that previously estimated with usage of the model with constant adiabatic index and without considering condensation as a factor affecting on pressure in impact-produced clouds.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"249 ","pages":"Article 105942"},"PeriodicalIF":1.8,"publicationDate":"2024-07-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141853339","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Laboratory testing of desiccation crack growth in terrestrial Martian analog environments using digital image correlation","authors":"Ali Ettehadi ,&nbsp;Maksym Chuprin ,&nbsp;Mehdi Mokhtari ,&nbsp;Robert C. Anderson","doi":"10.1016/j.pss.2024.105933","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105933","url":null,"abstract":"<div><p>The unique geologic features of raised ridges and polygonal cracks filled with multiple layers of cement observed in Gale and Jezero craters on Mars have origins that remain uncertain due to limited knowledge and measurement techniques. This study hypothesizes that these cracks result from the volumetric shrinkage of clay fabric due to dehydration and salinity fluctuations in ancient Martian lakes. The research aims to quantify the shrinkage of terrestrial simulants with varying mineral compositions analogous to those found at Gale Crater and Jezero Crater under diverse desiccation conditions. By simulating Martian regolith using the Rocknest soil simulant and examining historical aqueous conditions through sedimentary rock analogs, this study provides new insights into Martian geological structures. The extent and rate of shrinkage in simulant samples were quantified using ImageJ, while strain localization and propagation were measured using the Digital Image Correlation (DIC) technique until full desiccation crack patterns developed. Laboratory testing revealed that desiccation cracks tend to form polygonal patterns, which are patently similar to the polygonal patterns observed in some regions of Mars. However, not all simulants produced visible cracks, with some producing linear rather than polygonal patterns. Key findings indicate that higher temperatures result in wider and deeper cracks, while lower temperatures decrease crack density and length. Increased initial water content leads to more extensive cracking, with higher crack density and length per unit area. Sodium chloride and sodium sulfate significantly impact desiccation cracking, with low concentrations stabilizing the soil and high concentrations promoting extensive cracking. Smectite-rich samples exhibit extensive cracking, and tensile strain distribution during evaporation is non-uniform, influencing crack development based on sample properties and drying conditions. These insights enhance our understanding of polygonal crack formation on Mars, improving Mars sample return missions and informing the design of robust exploration equipment.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"248 ","pages":"Article 105933"},"PeriodicalIF":1.8,"publicationDate":"2024-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141593590","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Spectrometer to explore isotopologues of lunar volatiles on Luna-27 lander","authors":"Viacheslav Meshcherinov ,&nbsp;Iskander Gazizov ,&nbsp;Viktor Kazakov ,&nbsp;Maxim Spiridonov ,&nbsp;Yuri Lebedev ,&nbsp;Imant Vinogradov ,&nbsp;Mikhail Gerasimov","doi":"10.1016/j.pss.2024.105935","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105935","url":null,"abstract":"<div><p>The study of volatiles and the search for water are the primary objectives of the Luna-27 mission, which is planned to land on the south pole of the Moon in 2028. Here we present the tunable Diode Laser Spectrometer (DLS-L) that will be onboard the lander. The DLS-L will perform isotopic analysis of volatiles that are pyrolytically evolved from regolith. This article dives into the design of the spectrometer and the characterisation of isotopic signature retrieval. We look forward to expanding our knowledge of Lunar geochemistry by measuring D/H, ¹⁸O/¹⁷O/¹⁶O, ¹³C/¹²C ratios <em>in situ</em>, which would be the one-of-a-kind direct study of the lunar soil isotopy <em>without</em> sample contamination.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"248 ","pages":"Article 105935"},"PeriodicalIF":1.8,"publicationDate":"2024-07-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141593589","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An inorganic silicate simulant to represent the interior of enceladus","authors":"R.E. Hamp,&nbsp;K. Olsson-Francis,&nbsp;S.P. Schwenzer,&nbsp;V.K. Pearson","doi":"10.1016/j.pss.2024.105934","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105934","url":null,"abstract":"<div><p>Enceladus, an icy moon of Saturn, consists of an ice shell, global subsurface ocean and a silicate interior. By sampling plume material, the Cassini spacecraft found evidence of ongoing water-rock reactions between the silicate interior and the subsurface ocean. These data showed that these reactions provide a source of bioessential elements to the ocean, making Enceladus one of the leading astrobiological targets in our Solar System. Understanding these water-rock reactions is critical in understanding the potential habitability of Enceladus. To study these reactions experimentally, a chemical simulant to represent the contemporary silicate interior of Enceladus has been designed. Based on the available interpretations of Cassini data about the density, chemical composition, and aqueous alteration of the interior, the chosen starting point for the simulant is a CI chondrite. However, Enceladus is still undergoing active aqueous alteration, thus its silicate mineral assemblage cannot have reached the fully altered assemblage seen in a CI chondrite. To account for this, adaptations have been made to a CI chondrite mineral assemblage, extrapolating back to an assemblage of less aqueously altered minerals whilst maintaining the same chemical composition in terms of major oxide phases. Thus, the chemical and mineralogical composition of this simulant represents a best estimate of the silicate components in the ongoing water rock interactions on Enceladus today.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"248 ","pages":"Article 105934"},"PeriodicalIF":1.8,"publicationDate":"2024-07-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0032063324000989/pdfft?md5=ec206c3a8d3bac236ce8245834ef160b&pid=1-s2.0-S0032063324000989-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141593588","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Exploring the astrobiological potential of rock varnish from a mars analogue field site of Ladakh, India","authors":"Amritpal Singh Chaddha ,&nbsp;Anupam Sharma ,&nbsp;Narendra Kumar Singh ,&nbsp;Sheikh Nawaz Ali ,&nbsp;P.K. Das ,&nbsp;S.K. Pandey ,&nbsp;Binita Phartiyal ,&nbsp;Subodh Kumar","doi":"10.1016/j.pss.2024.105932","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105932","url":null,"abstract":"<div><p>Rock varnish, a dark-coloured natural feature rich in manganese (Mn), iron (Fe), and clay minerals that forms on rock surfaces and subsurface rock fractures in extremely dry and cold environments, is believed to provide nutritional support to microbiota. Because varnish supports an extensive microbial community, this rock coating is considered a substrate for potential microbial life to thrive in extreme environments on Earth. Although research in the past decades have advanced understanding of the varnish microbiome, little is known about this microbial community in settings that are high altitude (lower oxygen), dry, and cold. We present here new morphological, chemical, and rock magnetic results of rock varnish from this environmental setting, the Ladakh, a potential analogue site for life in extreme environments. Our results include the presence of putative magnetofossils-in the form of nanochains present in the rock varnish layer. Further, the higher concentrations of oxidised Mn⁴⁺ and carboxylic acid functionality on the varnish surface revealed organic signatures. These collective results point towards the enriched concentration of magnetic minerals on the varnish layer that are possibly sourced through biotic forms. Consequently, the rock varnish can serve as an archive of ancient environmental records, as well as a potential geomaterial for astrobiological studies from the Martian analogue field location of Ladakh, which needs to be explored further for extensive biogeochemical studies.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"248 ","pages":"Article 105932"},"PeriodicalIF":1.8,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141444673","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Spectral ratioing of Afρ to constrain the dust particle size distribution of comets","authors":"Nico Haslebacher ,&nbsp;Nicolas Thomas ,&nbsp;Raphael Marschall","doi":"10.1016/j.pss.2024.105925","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105925","url":null,"abstract":"<div><p>A numerical model of cometary dust environments is used to gain a deeper understanding of the relationship between the brightness (<span><math><mrow><mi>A</mi><mi>f</mi><mi>ρ</mi></mrow></math></span>) and the dust particle size distribution in the coma. Specifically, the spectral ratio of <span><math><mrow><mi>A</mi><mi>f</mi><mi>ρ</mi></mrow></math></span>(425 nm)<span><math><mo>/</mo></math></span> <span><math><mrow><mi>A</mi><mi>f</mi><mi>ρ</mi></mrow></math></span>(900 nm) is modelled for a wide range of parameters and tied to the power-law index. The studied parameters are dust composition, terminal outflow velocity and the dust production rate day–night asymmetry. We find that the spectral ratio of <span><math><mrow><mi>A</mi><mi>f</mi><mi>ρ</mi></mrow></math></span> modelled at 425 nm and 900 nm correlates with the power-law index of the particle size distribution. This method could be used to place constraints on the dust size distributions of comets and as a result improve the use of <span><math><mrow><mi>A</mi><mi>f</mi><mi>ρ</mi></mrow></math></span> as a proxy for cometary activity. Optically red dust indicates that the scattering is dominated by large particles.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"248 ","pages":"Article 105925"},"PeriodicalIF":2.4,"publicationDate":"2024-06-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0032063324000898/pdfft?md5=df2b3c75344d9943e184d7167cceca05&pid=1-s2.0-S0032063324000898-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141329258","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Clay mineralogy in west Chryse Planitia, Mars: Comparison with present and future landing sites","authors":"Jeremy Brossier,&nbsp;Francesca Altieri,&nbsp;Maria Cristina De Sanctis,&nbsp;Alessandro Frigeri,&nbsp;Marco Ferrari,&nbsp;Simone De Angelis,&nbsp;Enrico Bruschini,&nbsp;The Ma_MISS team","doi":"10.1016/j.pss.2024.105924","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105924","url":null,"abstract":"<div><p>On Mars, the well-known crustal dichotomy marks the boundary between the old southern highlands and the younger northern lowlands. Among these lowlands, Chryse Planitia resembles a quasi-circular basin surrounded by several highlands, and blends into Acidalia Planitia, another flat lowland located farther north. The transition area between these highlands and the Chryse basin is often designated as “<em>circum-Chryse Planitia</em>”, and is the terminus for many outflow channels. Infrared datasets display several sites therein with extensive clay-bearing outcrops, further testifying for aqueous activity on early Mars – notably around Mawrth Vallis, Oxia Planum and Xanthe Terra. In this study, we investigate clay-bearing outcrops identified along the western margins of circum-Chryse basin, often overlooked in the Martian literature. We also compare them with outcrops found in other regions along the crustal dichotomy and relevant in the Martian literature, such as Oxia Planum, Mawrth Vallis and Nili Fossae. Investigating such deposits is crucial for astrobiological perspectives, as they are appealing targets to search for organic compounds possibly stored throughout the rocks and soils. Fe,Mg-rich clays generally result from the interaction of liquid water with rocks under low temperatures, moderate pH levels and neutral to reducing conditions, factors favorable for life. Here, the clay minerals detected in west Chryse Planitia are consistent with either ferrosaponites or vermiculites associated with hydrobiotite, as recently inferred in Oxia Planum and north Xanthe Terra. Diverse alteration pathways might be involved based on either of these clay species. The clay-bearing rocks crop out in isolated hills in Lunae Planum, and along inverted channels and small craters in Tempe Terra. Further geologic investigations in circum-Chryse Planitia should certainly provide new clues on their origin and weathering conditions, while supporting the upcoming ExoMars rover mission and other future explorations.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"247 ","pages":"Article 105924"},"PeriodicalIF":2.4,"publicationDate":"2024-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141289866","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A model of radio scintillations in the deep Venus atmosphere: Application to the DAVINCI probe","authors":"Ralph D. Lorenz","doi":"10.1016/j.pss.2024.105923","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105923","url":null,"abstract":"<div><p>Power fluctuations have been noted on radio signals propagating through the Venus atmosphere since the very first descent probe there (Venera 4) and have been observed as a routine feature in radio occultations, where the grazing ray geometry amplifies the effect of refractive scattering structures. Motivated by DAVINCI and other missions currently in development, a physical model of refraction variations in the Venus atmosphere is developed using the VEGA-2 high-resolution temperature profile down to the surface and other data, which suggest several distinct layers of more intense scattering. The resultant modeled radio scintillations are compared with observed scintillations and assessed for the DAVINCI relay link. High-time-resolution radio signal power measurements on the DAVINCI radio link promise to be an interesting probe of the Venus atmosphere.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"247 ","pages":"Article 105923"},"PeriodicalIF":2.4,"publicationDate":"2024-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141263899","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Automatic lunar dome detection methods based on deep learning","authors":"Yunxiang Tian,&nbsp;Xiaolin Tian","doi":"10.1016/j.pss.2024.105916","DOIUrl":"https://doi.org/10.1016/j.pss.2024.105916","url":null,"abstract":"<div><p>Lunar domes are common structures on the lunar surface and are important for studying the geological evolution of the moon. The distribution of spatial frequencies of lunar domes provides significant evidence for the evolution of lunar volcanoes. In recent years, deep learning methods have been rapidly developing in many fields. However, most of the existing dome detection algorithms use manual or semi-automatic traditional methods. In this paper, we propose an automatic deep learning recognition method to simplify the traditional dome identification process, which is an end-to-end detection method. We built a lunar dome dataset using digital elevation model data and compared eleven advanced deep learning target detection algorithms, which include three types of detection architecture. The region of Marius Hills was selected for validation to evaluate method performance. By comparing the results with manual identification, the proposed method has an identification precision of 88.7%. In addition, we detected 12 unrecorded potential domes/cones. The morphological characterization and visualization results indicate that the detected features may be domes/cones and our method may provide novel dome detection.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"248 ","pages":"Article 105916"},"PeriodicalIF":1.8,"publicationDate":"2024-05-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141438949","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"3D porosity, flow, and transport characteristics of two L chondrites reveal wet accretion-related cosmic web-like porosity","authors":"A.-J. Soini ,&nbsp;I.T. Kukkonen ,&nbsp;H. Suhonen ,&nbsp;B. Lukić ,&nbsp;A.V. Luttinen","doi":"10.1016/j.pss.2024.105915","DOIUrl":"10.1016/j.pss.2024.105915","url":null,"abstract":"<div><p>Porosity, with its structure-dependent flow properties (permeability and tortuosity) and transport properties (thermal conductivity and thermal diffusivity), is closely related to the accretion, thermal metamorphism, and associated hydrothermal alteration of ordinary chondrite (OC) parent bodies. Using synchrotron radiation microtomography (SRμCT), we reveal the varying porosity structures in two L chondrite falls of low (Mezö-Madaras L3.7) and high (Bath Furnace L6) petrologic types and quantify porosity properties, such as shape and connectivity, and related effective permeability and tortuosity factor. Although the two specimens demonstrate similar effective permeabilities, they exhibit significantly different tortuosity factors and textures of porosity, which include notable differences in void throat diameters, complexity and density of the interconnected void network, heterogeneity in void distribution, and the extent of primary and secondary porosity. The complex relationships among porosity, permeability, tortuosity, and thermal conductivity can be explained by the varying void arrangements related to varying grain sizes among the petrologic types of OCs, which in turn reflect their varying evolutionary paths.</p><p>Electron microprobe and attached energy-dispersive X-ray spectrometer reveal signs of hydrothermal alteration in both petrologic types. High-energy SRμCT imaging (0.65 μm voxel size) reveals the presence of a new microporosity substructure resembling a microscopic cosmic web, which may be linked to fluid-assisted metamorphism and hydrothermal alteration during wet accretion of the parent body. Furthermore, the proportion of this continuous porosity may be related to the temperatures associated with different petrologic types, and the wet accretion model may resolve the lack of correlation between petrologic types and porosity of OCs. Finally, the uncovered cosmic web-like microporosity structure may explain the observed concurrent high thermal conductivity, low permeability, and high porosity of the high-petrologic-type OCs.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"247 ","pages":"Article 105915"},"PeriodicalIF":2.4,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0032063324000795/pdfft?md5=2b20e0684139e73c0b6034d0b9071eea&pid=1-s2.0-S0032063324000795-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141130337","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}