JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
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2024
·Vol. 129
·期 4
·e2023JE008031
·
IF 3.9
Xinyi Xiang,Peixin Du,Binlong Ye,Hongling Bu,Dong Liu,Jiacheng Liu,Jian Hua,Xiaolong Guo
Ferrihydrite, a nanocrystalline iron (oxyhydr)oxide mineral, is widely distributed in soils and sediments on Earth and is probably an important component and/or precursor of widespread nanophase iron minerals on Mars. Terrestrial ferrihydrite often co-occurs with amorphous silica and/or contains a certain amount of Si in its structure. However, it remains ambiguous how environmental Si concentration affects the formation-evolution and structure-spectral features of ferrihydrite in the Fe(III)-Si systems. To this end, hydrolysis experiments were carried out for Fe-Si systems at an unprecedentedly wide range of initial Si/(Fe + Si) molar ratios (0–0.80), followed by characterizing the products detailly. X-ray diffraction, Fourier transform infrared (FTIR) spectroscopy, Raman spectroscopy, Mössbauer spectroscopy, and transmission electron microscopy results showed that at Si/(Fe + Si) molar ratios ≤0.30, the main phase of the products was ferrihydrite, of which the unit cells enlarged, the crystallinity decreased, and the existing state of Fe changed with increased Si contents; at Si/(Fe + Si) molar ratios ≥0.40, ferrihydrite was no longer formed and a novel amorphous Fe-O-Si phase was instead obtained, with the excess Si forming amorphous silica. The visible and near-infrared spectroscopy, the most powerful tool to detect hydrous minerals on the surface of Mars at global or regional scales, showed weakness in identifying ferrihydrite-like materials obtained in the Fe-Si systems. Raman spectroscopy can identify ferrihydrite and Si-containing ferrihydrite but cannot differentiate between them. Mössbauer spectroscopy showed great potential in both identifying and differentiating between ferrihydrite and Si-containing ferrihydrite, and thus can be used to characterize the poorly ordered iron (oxyhydr)oxides on Mars. Key Points Hydrolysis experiments of Fe(III)-Si systems were performed at an unprecedentedly wide range of initial Si/(Fe + Si) molar ratios (0∼0.80) The environmental Si concentration controls the formation and evolution of ferrihydrite in the Fe(III)-Si systems Mössbauer spectroscopy shows great potential in identifying and differentiating between ferrihydrite-like materials Plain Language Summary On the surface of ancient Mars where liquid water was available, Fe-Si hydrolysis systems were likely common as a result of the high abundances of Fe and Si in the crust of Mars. By performing hydrolysis experiments of Fe-Si systems at an unprecedented wide range of Si/(Fe + Si) molar ratios, we found that the hydrolysis products of Fe-Si systems varied among combinations of ferrihydrite, Si-containing ferrihydrite, an unknown Fe-O-Si phase, and amorphous silica. We also found that the visible and near-infrared reflectance spectroscopy, the most powerful tool to remotely detect hydrous minerals on the surface of Mars at global and regional scales, showed weakness in identifying ferrihydrite, Si-containing ferrihydrite, and the novel Fe-O-Si phase; Raman can be used to identify ferrihydrite-like materials but cannot be used to differentiate between ferrihydrite and Si-containing ferrihydrite; mid-infrared spectroscopy can differentiate ferrihydrite from Si-containing ferrihydrite and the novel Fe-O-Si phase; Mössbauer spectroscopy (recorded at varied temperatures) provided clues to identifying and further differentiating between ferrihydrite-like materials and thus holds great potential for detecting Fe/Si-rich phases on the surface of Mars.
研究领域:
地质学
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行星科学
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矿物学
✓ 已验证
DOI
高影响因子
Communications Earth & Environment
·
2022
·Vol. 3
·期 1
·1-10
·
IF 7.29
Li Dongdong,Zhao Yu-Yan Sara,Meslin Pierre-Yves,Vals Margaux,Forget François,Wu Zhongchen
The high perchlorate (ClO 4 − ) to chloride (Cl − ) ratios observed at the Phoenix landing site, northern polar region of Mars, have been puzzling since detection. However, a lack of understanding of perchlorate-chloride-water systems under cryogenic conditions makes it difficult to assess ClO 4 − /Cl − ratios during deliquescence-related processes. Here we quantitatively evaluate ClO 4 − /Cl − fractionation in deliquescence-induced brines of magnesium- and calcium-perchlorate-chloride salt mixtures under subzero conditions, by measuring solubility data and constructing temperature-dependent thermodynamic models. We find that under specific relative humidity (RH) and temperature ( T ) conditions, deliquescence of perchlorate-chloride mixtures may form brines with fractionated ClO 4 − /Cl − signatures. Appropriate RH -T , water-limited conditions, and aeolian processes are required to produce and preserve the elevated ClO 4 − /Cl − signatures in soils. Under the present climate, the north polar region can support ClO 4 − /Cl − fractionation and potentially enrich perchlorate for longer periods on global Mars. This highlights the uniqueness of Mars’ arctic environment and its implications for modern habitability.
研究领域:
地球科学
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化学
✓ 已验证
DOI
高影响因子
Planetary Science Journal
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2025
·Vol. 6
·期 3
·55
·
IF 4.3
Erbin Shi,Xiaojia Zeng,Jian Chen,Enming Ju,Zongcheng Ling
Calcium sulfates are widely distributed in Gale crater and Endeavour crater on Mars. However, the mole ratios of Ca2+ and SO3 in some Sr–Ba-rich sulfate veins are less than 1. This indicates that there may be additional solid solution phases on Mars, including Ca–Sr, Ba–Sr, and Ca–Ba sulfates, which, on Earth, are typically found in marine environments. In this study, we synthesized a series of Ca–Sr, Ba–Sr, and Ca–Ba sulfate solid solutions in the laboratory. These synthesized solid solutions were then characterized using various techniques, including X-ray powder diffraction (XRD), Raman, mid-infrared, and visible and near-infrared. Our results show that the XRD and Raman spectra of Ca–Sr and Ba–Sr sulfates varied with their cation contents. In particular, the linear relationships (R2 ≥ 0.98) between the mole ratios of cation ions and peak positions of {{\rm{SO}}}_{4}^{2{-}} tetrahedron (v1) in Raman spectra were obtained. The mole content of Ca2+, Sr2+, and Ba2+ can be precisely constrained in Ca–Sr, Ba–Sr, and Ca–Ba sulfate solid solution phases through linear relationships, respectively. These results are the experimental basis for analyzing in situ detection data (e.g., SHERLOC, SuperCam, and Oxia planum) and can be used to precisely constrain the mineral phases of calcium sulfate veins on Mars.
研究领域:
地质学
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行星科学
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光谱学
✓ 已验证
产品关联
DOI
高影响因子
ACS Earth and Space Chemistry
·
2024
·
IF 2.9
Junqi Ren,Wenshuo Mao,Zhongchen Wu,Xiaohui Fu,Qiyuan Hou,Mingyu Chen,Ziwei Fu
The Martian atmosphere and surface materials can be impacted by electrochemical reactions that occur during dust activity on Mars. Prior research has shown that in the dry Martian surface environment, electrostatic discharge (ESD) can generate oxychlorine along with converting CO2 to carbonate dust. To comprehend the carbon and chlorine cycles on Mars, research on carbonates and oxychlorine is crucial, as is investigating the effects of coexisting minerals. In support of this work, precise methods for measuring ESD reactions are needed. Herein, ESD reactions on chloride (NaCl) and potential coexisting minerals SiO2 or TiO2 were investigated under simulated Martian atmosphere conditions, and Raman spectroscopy was used to measure trace products. Based on Raman measurements, the influences of coexisting minerals on the production of carbonates and oxychlorine during ESD reactions were investigated. Our findings suggest that Raman spectroscopy has sensitive quantitative detection capabilities in aqueous solutions, offering a useful technique for the quantitative detection of laboratory products. Carbonate continuously accumulated with increasing discharge time, with 14–22 times greater yield (1.43–4.77‰ and 5% error) than perchlorate (0.10–0.24‰ and 20% error) and 5–16 times greater yield than chlorate (0.28–0.44‰ and 20% error). The yields of the above products were found to depend on the type, content, and particle size of coexisting minerals. Our findings are crucial for understanding the current geological history, atmospheric evolution, and substance cycling on Mars, as well as for retracing the development of Martian atmospheric and hydrological environments.
研究领域:
行星科学
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地质学
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化学
✓ 已验证
DOI
高影响因子
PHYSICA SCRIPTA
·
2025
·Vol. 100
·期 2
·025409
·
IF 2.6
Xiaoyu Wang,Ziyuan Wang,Erbin Shi,Zongcheng Ling
Searching for life on Mars can help us understand the origins and evolution of life, and it has always been a primary scientific goal of Mars exploration missions by different countries. Raman spectroscopy has numerous advantages in detecting different materials, such as gathering chemical composition and crystal structure, specifically, ultraviolet Raman spectroscopy which is especially suitable for identifying organic compounds has been deployed on Mars. In this study, an independent UV Raman spectroscopy system is built to explore the potential of ultraviolet Raman spectroscopy in planetary exploration and astrobiology. Based on this system, a ground-based Raman reference library was established, including 41 minerals and 21 organic compounds related to Martian biosignatures. The results indicate that the self-built UV Raman system can identify significant characteristic peaks in different materials that would provide valuable and good references for identifying organics on Mars.
研究领域:
天体生物学
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行星科学
✓ 已验证
DOI
高影响因子
ACS Earth and Space Chemistry
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2025
·
IF 2.9
Qi Tao,Yonglei Zhang,Tianqi Zhang,Xiaorong Qin,Binglong Ye,Hongping He,Sridhar Komarneni
Over the past decade, remote sensing exploration has revealed widespread detection of clay minerals in Noachian terrains (>3.7 Ga) on Mars, suggesting a period of active near-surface water–rock interaction. The in-depth characterization of the crystal structure and chemistry of laboratory-synthesized smectite minerals with varying compositions offers a unique perspective to further constrain their formation mechanism, environmental conditions, and the climate of early Mars. This study synthesized smectites with varying Fe/Mg ratios to compare their near-infrared (NIR) spectral characteristics with those of representative areas on Mars. The study revealed that the characteristic metal–OH (M–OH) band in the range of 2270–2320 nm shifted toward longer wavelengths as the octahedral Fe3+ content decreased. When the octahedral Fe/Mg ratio was close to 1, the position of M–OH was similar to that of Mg-smectite (saponite), indicating that although the M–OH band of smectite is located at ca. 2308–2312 nm, it may still contain a significant amount of octahedral Fe3+. This suggests that there are likely still many Fe-smectites in Mg-rich smectite outcrops (ca. 20% as in the literature) on the Martian surface. Furthermore, correlation analysis between the smectite layer stacking order index (V/P) and the second-order derivative band intensity ratio (Deriv2 ratio) showed that when the Deriv2 ratio is small (generally <8), smectite has a relatively high degree of layer stacking order. When the Deriv2 ratio is >10 and tends toward infinity (+∞), the layer stacking order of smectite is very low. The above results suggest that the crystal chemical characteristics of smectites should be carefully studied when analyzing the mineral composition of the Mars surface using remote sensing or in situ NIR spectra. Smectites on Mars generally exhibit a high layer stacking order, indicating the presence of a relatively long-term warm and humid climate in Martian history. However, later alteration processes can significantly reduce their crystallinity.
研究领域:
地质学
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行星科学
✓ 已验证
产品关联
DOI
高影响因子
Remote Sensing
·
2024
·Vol. 16
·期 5
·820
·
IF 4.2
Yiheng Liu,Changqing Liu,Yanqing Xin,Ping Liu,Ayang Xiao,Zongcheng Ling
With the development of technology and methodologies, Raman spectrometers are becoming efficient candidate payloads for planetary materials characterizations in deep space exploration missions. The National Aeronautics and Space Administration (NASA) already deployed two Raman instruments, Super Cam and SHERLOC, onboard the Perseverance Rover in the Mars 2020 mission. In the ground test, the SHERLOC team found an axial offset (~720 μm) between the ACI (Autofocus Context Imager) and the spectrometer focus, which would obviously affect the acquired Raman intensity if not corrected. To eliminate this error and, more importantly, simplify the application of Raman instruments in deep space exploration missions, we propose an automatic focusing method wherein Raman signals are optimized during spectrum collection. We put forward a novel method that is realized by evaluating focus conditions numerically and searching for the extremum point as the final focal point. To verify the effectiveness of this method, we developed an Auto-focus Raman Probe (SDU-ARP) in our laboratory. This method provides a research direction for scenarios in which spectrometers cannot focus on a target using any other criterion. The utilization of this auto-focusing method can offer better spectra and fewer acquisitions in focusing procedure, and the spectrometer payload can be deployed in light-weight bodies (e.g., asteroids) or in poor illumination conditions (e.g., the permanently shadowed region in the Lunar south polar area) in deep space exploration missions.
研究领域:
天文学
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仪器科学
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空间科学
✓ 已验证
DOI
高影响因子
JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
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2020
·Vol. 125
·期 12
·e2020JE006590
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IF 3.717
Peixin Du,Peng Yuan,Jiacheng Liu,Yixuan Yang,Hongling Bu,Shun Wang,Junming Zhou,Hongzhe Song,Dong Liu,Joseph R. Michalski,Chengshuai Liu
Allophane, a common component on Earth and a probable constituent of the amorphous component on Mars, is closely associated with Fe in the form of structural Fe and/or iron (oxyhydr)oxide coatings. However, until now, the formation and evolution of allophane as products of environmental Fe concentrations have rarely been studied. We investigated allophane precipitation from gels with different Fe/(Fe + Al) molar ratios ( n , 0 ≤ n ≤ 1.0). X-ray diffraction patterns and Fourier transform infrared spectra of the products showed that allophane was nearly the only product at n ≤ 0.2 and that the crystallinity of Fe-rich allophane decreased with increasing n . Combined with the results of transmission electron microscopy and Mössbauer spectroscopy, Fe was found to be mainly incorporated into the gibbsite-like sheet of allophane, forming clusters; the highest Fe-for-Al substitution content was roughly estimated to be 20 mol.%. As n increased further, the formation of allophane was increasingly suppressed, and the Fe phases began to separate from the Al-Si phases, resulting in mixtures of incipient allophane and incipient akaganeite and finally akaganeite. The near-infrared spectroscopic data (1.2–2.6 μ m) of the products showed incapability in identifying poorly ordered minerals in Al-Si-Fe systems, while the features in the range of 0.4–1.2 μ m were powerful for studying iron occurrence in the products. These findings not only offer insights into the formation, evolution and geological role of allophane in Al-Si-Fe systems on Earth but also help constrain the paleoenvironment of locations where allophane and akaganeite co-occur on Mars. Key Points Environmental Fe concentrations control the formation and evolution of allophane in Al-Si-Fe systems Near-infrared spectra (1.2–2.6 μ m) show incapability in identifying short-range ordered minerals in Al-Si-Fe systems Co-occurrence of allophane and akaganeite would constrain the local palaeoenvironment on Mars
研究领域:
地质学
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行星科学
✓ 已验证
DOI
高影响因子
SEPARATION AND PURIFICATION TECHNOLOGY
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2025
·
IF 9
Jinzhao Guan,Ming Lin,Zhiliang Tan,Yu-jun Li,Xingkai Duan,Shifang Ma,Yang Wang,Zhongning Shi,Hui Dong
Mars is a long-term target for human exploration in the future. On the basis of the demands of space exploration and in situ resource utilization, Martian soil simulant NEU Mars-1 was applied for metal extraction and oxygen preparation in 50.9 wt% KF-49.1 wt% AlF 3 molten salt at 750 °C, and the dissolution and electroreduction behaviors of Martian soil simulants were studied via the isothermal saturation method and electrochemical techniques, respectively. The results revealed that the concentrations of SiO 2 , Fe 2 O 3 , and TiO 2 in the molten salt reached 6.09 %, 0.25 %, and 0.17 %, respectively, when the dissolution was in equilibrium. The reduction processes of various ions in Martian soil simulants were as follows: Fe(III) was first reduced to Fe(II) and Fe, Si(IV) was reduced to Si(II), and Fe(II) was reduced to Fe, and finally, Al and Si were codeposited. NEU Mars-1 was electrolyzed with an Fe-Ni anode and liquid Al as the cathode in molten salt. The purity of the anode gas O 2 was 95.41 %, whereas an Al-Si-Fe-Ti alloy containing 12.13 wt% Si, 3.00 wt% Fe and 0.17 wt% Ti was obtained at the cathode.
研究领域:
材料科学
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化学工程
·
空间探索
✓ 已验证
产品关联
DOI
高影响因子
ACTA ASTRONAUTICA
·
2024
·
IF 3.1
Zilong Zhao,Jun Chen,Zhichao Yang,Chenbin Zhao,Yuxin Wei,Weidong Wang,Hong Qiao,Wen Ao
Mg-based nanofluid fuel is a promising fuel for propulsion system in Mars exploration . In this study, Mg-based nanofluid fuel were prepared by one-step method, and the effect of Mg(magnesium) content, Mg size(68 μm,110 μm,175 μm), and oleic acid (OA) on droplet ignition and combustion under the atmosphere of 90 % CO 2 and 10 % O 2 were investigated. According to the TG-DSC results, 68 m Mg particles under CO 2 had the highest exothermic efficiency of 4472 J/g. The combustion of Mg/OA/kerosene droplets consists of five stages: ignition, d 2 -law combustion, micro-explosion, vapor flame extinguishment, and agglomerate explosion. The ignition delay time of Mg (68 μm, 5 %)/kerosene is 0.045s, which is half that of kerosene (0.0890s). The agglomerates explode violently and emit a brilliant white light at the end of the Mg-based nanofluid fuel combustion . The explosive effect of Mg agglomerates diminishes as the Mg content increases. The rate of combustion decreases with increasing particle size. In the sample with added oleic acid, Mg (68 μm, 5 %)/OA/kerosene shows the best combustion rate of 0.6320 mm 2 /s. Finally, a numerical model for the combustion of Mg-based nanofluid fuel droplets is proposed. The predictions are within 2 % of the experimental results. The findings are expected to explore future in-situ utilization of CO 2 on the Mars surface .
研究领域:
能源科学
·
材料科学
✓ 已验证
DOI
高影响因子
PLANETARY AND SPACE SCIENCE
·
2014
·
IF 1.63
Scott L. Murchie,Daniel T. Britt,Carle M. Pieters
Phobos occupies a unique position physically, scientifically, and programmatically on the road to exploration of the solar system. It is a low-gravity object moderately inside the gravity well of Mars. Scientifically, it is both an enigma and an opportunity: an enigma because the origins of both it and Deimos are uncertain, and provide insights into formation of the terrestrial planets ; and an opportunity because Phobos may be a waypoint or staging point for future human exploration of the Mars system. Phobos is a low albedo , spectrally bland body with a red-sloped continuum. It appears similar to D-type objects more commonly found in the outer asteroid belt and Jovian space ( Rivkin et al., 2002 ), but occurs in an orbit that is difficult to explain by capture ( Burns, 1992 ). It might have a primitive composition like that inferred for outer solar system objects or it could be related to Mars and, for example, be composed of Martian basin ejecta . Regardless, Phobos has acted as a witness plate to Martian debris over the age of the solar system. The moons may possibly be a source of in situ resources that could support future human exploration in circum-Mars space or on the Martian surface. in situ compositional analyses can address many questions relevant to preparation for future human exploration. Sample return resolves those questions while also enabling detailed analyses in terrestrial laboratories to address higher order questions, many of which have not yet been asked.
研究领域:
行星科学
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天体化学
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空间探索
·
太阳系动力学
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陨石学
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原位资源利用
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比较行星学
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深空探测
✓ 已验证
DOI
高影响因子
危险品化学品经营许可证（带存储）