Planetary and Space Science最新文献

{"title":"Lunar Mare Ingenii: A comprehensive multi data study unravelling composition, chronology and terrain dynamics","authors":"Neeraja C R ,&nbsp;Arivazhagan S ,&nbsp;Karthi A","doi":"10.1016/j.pss.2025.106046","DOIUrl":"10.1016/j.pss.2025.106046","url":null,"abstract":"<div><div>The compositional, chronological, topographical, and morphological features of Mare Ingenii, an impact basin situated in the northwest part of the South Pole-Aitken basin (SPA) are cha racterized using different orbital remote sensing data. Examining the chemical characteristics, spectral signatures, age, and surface features help to elucidate the basin's formation process and its volcanic evolution. In the present study, Chandrayaan-1 Moon Minerology Mapper (Ch-1 M³) data is used to prepare Standard Band Ratio (SBR), Optical Maturity (OMAT), 1000 and 2000 nm Integrated Band Depth (IBD) color composite images to map different lithologies and mafic signatures of the basin. Chandrayaan-2 Imaging Infrared Spectrometer (Ch-2 IIRS) data is used to derive 1000 and 2000 nm IBD and result is validated with M³ derived images. Minerals like olivine, pyroxene, plagioclase, spinel, and ilmenite are identified and validated through spectral studies. The FeO wt.% map from Kaguya and the TiO₂ map from the Lunar Reconnaissance Orbiter Camera - Wide Angle Camera (LROC WAC) were used to obtain FeO and TiO₂ abundances. These were then compared with abundances derived from M³ data to validate the compositional analysis. The present study identified 19 mare units in the Ingenii basin using variations in TiO₂, FeO, and IBD color composite maps. Crater Size-Frequency Distribution (CSFD) technique has been employed to obtain the age of each unit and it ranges from 3.8 to 2.3 Ga and the results well correlated with previous studies. It is thus evident that Mare Ingenii has been affected by a prolonged period of mare volcanism along with a few non-mare basaltic surfaces that have been identified, including rille-related lava flows and O'Day impact melt sheets. The basin was flooded mainly by low to very low Ti basalts of the Imbrian period and patches of intermediate Ti basaltic emplacement happened during the Eratosthenian period. The topography of the basin is delineated by using Lunar Orbiter Laser Altimeter (LOLA) data and an outer ring of 600 km is mapped in this study. Morphological features such as rille, wrinkle ridge, graben, swirls, O'Day impact melt, and V-shaped features are identified using Kaguya Terrain Camera (TC) and LROC data which can offer understanding into the basin's past volcanic and cratering process. The results suggest that Mare Ingenii possesses a prolonged volcanic history and the mare is dominated by low to very low Ti basalts sourced from olivine-ilmenite-pyroxene cumulates.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106046"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262395","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":"Practical exogeoconservation of Mars: Lessons from the Mars Desert Research Station, Utah","authors":"Clare Fletcher ,&nbsp;Martin Van Kranendonk ,&nbsp;Carol Oliver","doi":"10.1016/j.pss.2025.106038","DOIUrl":"10.1016/j.pss.2025.106038","url":null,"abstract":"<div><div>Of the planets in our solar system, Mars may be the most likely place to find evidence of life and learn about planetary evolution. However, in exploring Mars, we risk damaging sites of possible outstanding universal geoheritage value due to a lack of legal frameworks or practical guidelines. This study sought to develop practical exogeoconservation methods and test these at the Mars Desert Research Station (MDRS) over two crew rotations, totalling one month. However, there were several unanticipated challenges both in pre-mission planning and on-site, in-person exploration, making effective, practical exogeoconservation extremely challenging. This analogue study has implications for continued Mars exploration, as without practical exogeoconservation methods, we may risk the destruction of sites of possible outstanding universal geoheritage value on Mars. We find that exogeoconservation of Mars will require significantly more detailed information and study than is currently available. A key implication of this study is that sampling of potentially important outcrops should be reserved until after a whole area has been explored in-depth, to ensure the samples taken are both exceptional and common enough to allow for their removal. We also find that there is a role for geoconservation experts on Mars exploration teams to bring exogeoconservation principles to the forefront of Mars missions.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106038"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262392","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":"Mineralogy, geochemistry and morphology of Arctic gossans on Axel Heiberg Island, NU, Canada: Spectroscopic investigation and implications for Mars","authors":"Gaëlle Belleau-Magnat ,&nbsp;Myriam Lemelin ,&nbsp;Edward Cloutis ,&nbsp;Richard Léveillé","doi":"10.1016/j.pss.2025.106036","DOIUrl":"10.1016/j.pss.2025.106036","url":null,"abstract":"<div><div>Gossans are formed through the oxidation of sulfide ore deposits by fluids, such as meteoric water or hydrothermal solutions, leading to locally acidic conditions. In permafrost regions, gossans undergo seasonal chemical weathering after their initial formation (reactive gossans), potentially providing a sustained energy source for microbial activity. Arctic gossans are therefore considered valuable analogs for Martian paleo-hydrothermal systems and promising astrobiological targets. While hundreds of gossans have been identified in the Arctic, few have been studied in detail and even fewer using rover-compatible remote sensing techniques. This study aims to characterize the morphological profile of seven Arctic gossans located at Expedition Fiord (Axel Heiberg Island, Nunavut), as well as their geochemistry, mineralogy and organic carbon content using X-ray fluorescence, X-ray diffraction (XRD), Visible (VNIR) to thermal infrared (MIR-TIR) reflectance and Raman spectroscopy. Results showed a dominance of silicon, calcium and iron. Mineralogical analyses revealed gypsum and quartz as major phases, with variable amounts of silicates, sulfates, iron sulfides and iron oxyhydroxides. Raman spectroscopy detected organic carbon in most samples, up to 50 cm deep, in various organo-mineral complexes. XRD was the only technique to detect iron sulfides. VNIR-MIR-TIR reflectance and Raman spectroscopy provided mineralogical results consistent with XRD. All gossans displayed classical profiles, with alteration zones overlying primary sulfides, but showed diverse color and compositional stratification patterns. These variations suggest local mechanisms influence mineral and associated organic carbon distribution. Further investigations should focus on better understanding these local variations, which could guide the search for biosignatures in gossan-like features on Mars.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106036"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262393","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":"Comprehensive intercomparison of Martian dust optical depth datasets to assess agreement with Mars Climate Sounder observations","authors":"N.T. Martin ,&nbsp;A. Kleinböhl ,&nbsp;M. Slipski ,&nbsp;H.E. Gillespie ,&nbsp;J.H. Shirley ,&nbsp;M.J. Wolff ,&nbsp;M.D. Smith","doi":"10.1016/j.pss.2025.106035","DOIUrl":"10.1016/j.pss.2025.106035","url":null,"abstract":"<div><div>This study provides comprehensive intercomparisons of dust optical depths derived from Mars Climate Sounder on Mars Reconnaissance Orbiter with measurements from the orbiter instruments THEMIS on Mars Odyssey, CRISM on Mars Reconnaissance Orbiter, EMIRS on the Emirates Mars Mission, and from the surface-based instruments Pancam on the Spirit and Opportunity rovers and SSI on the Phoenix lander. We demonstrate good overall agreement between these dust optical depth datasets, in particular as these measurements were taken at different wavelengths (near IR to thermal IR) and with different measurement geometries (limb, downlooking from orbit, uplooking from the surface). To draw our conclusions, we use direct comparisons of co-located measurements from these instruments, plots of the dust optical depth differences averaged by latitude and Solar longitude, as well as modified Bland–Altman analysis that takes the measurement uncertainties into account. From the Bland–Altman analysis, we find that error estimates provided by the instruments reasonably represent the variability introduced by the two datasets but do not capture offsets. Based on our investigations, we propose potential physical causes, such as surface reflectance factor estimation and thermal contrast, for some of the observed differences. We find a linear relation of the differences in dust optical depth between MCS and the other instruments with derived MCS water ice optical depth. Taking this relation into account, together with a constant parameter that accounts for general offsets between the datasets, significantly reduces differences.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106035"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262391","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":"Optimal choice of closest approach distance for a comet flyby: Application to the Comet Interceptor mission","authors":"J. De Keyser ,&nbsp;N.J.T. Edberg ,&nbsp;P. Henri ,&nbsp;H. Rothkaehl ,&nbsp;V. Della Corte ,&nbsp;M. Rubin ,&nbsp;R. Funase ,&nbsp;S. Kasahara ,&nbsp;C. Snodgrass","doi":"10.1016/j.pss.2024.106032","DOIUrl":"10.1016/j.pss.2024.106032","url":null,"abstract":"<div><div>A comet flyby, like the one planned for the Comet Interceptor mission, takes place under conditions that remain largely unknown up to the moment of encounter. A detailed trajectory design phase, which includes verification of the technical limitations implied by the flyby geometry, precedes target comet selection. Thus the flyby velocity and the solar zenith angle at closest approach are known in advance. Solar irradiance and the neutral gas expansion speed can be estimated reasonably well. However, the comet outgassing rate, the dust production rate, and the solar wind conditions are only known within broader uncertainty margins. The present paper aims to optimally choose the one degree of freedom that is available for tuning the flyby conditions: the distance of closest approach. This choice is based on a simplified formalism that expresses, on one hand, the science return to be expected as a function of the closest approach distance, and, on the other hand, the risks implied by a close approach. This is done by performing Monte Carlo simulations over a large sample of possible comet flyby configurations, based on the expected probability distributions of the gas and dust production rates and the solar wind conditions, for different closest approach distances. For small flyby distances, a spacecraft has the opportunity to study the nucleus, the neutral gas coma, and the induced magnetosphere from up close, benefiting the science return. There is a trade-off to be made against the cometary dust collision risk, which becomes larger close to the nucleus. This trade-off is illustrated for the case of the Comet Interceptor main spacecraft and the two probes it plans to release. The change of the optimal flyby distance with gas and dust production rate, solar EUV flux, and flyby speed is discussed.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106032"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262389","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":"High resolution olivine abundance mapping in the Copernicus crater combining spectral data of Chandrayaan-1 M3 and Kaguya MI","authors":"Yehor Surkov ,&nbsp;Urs Mall ,&nbsp;Viktor Korokhin","doi":"10.1016/j.pss.2025.106039","DOIUrl":"10.1016/j.pss.2025.106039","url":null,"abstract":"<div><div>We present a technique for improving the spatial resolution of satellite spectrophotometric data of the Moon's surface using an artificial neural network. We demonstrate this approach using the high-spectral low-spatial resolution Moon Mineralogy Mapper (M³) spectrophotometer and the low-spectral high-spatial resolution Multiband Imager (MI) Kaguya datasets for super-resolution olivine mapping over the Copernicus crater. The super-resolution of spectral maps is achieved by correlating spectral data of these instruments using a multilayer perceptron. An important advantage of the method is the use of a single data frame from each dataset to study a particular lunar region. The obtained maps of the olivine abundance provide new spatial context of the investigated mineral distribution: olivine-rich surface units become visible primarily as flow tubes, lava ponds on the crater walls and boulder outcrops associated with high olivine content (up to 90 vol%) at the central peak of the investigated crater. The content of the olivine-reaches deposits of the area on the central peak reaches up to 35 vol % of the lunar regolith.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106039"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262394","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":"Compositional mapping and geological age of the mare basalts of the southern quadrangle of Moon","authors":"D. Paul ,&nbsp;S. Dhoundiyal ,&nbsp;A. Porwal ,&nbsp;G. Thangjam","doi":"10.1016/j.pss.2025.106034","DOIUrl":"10.1016/j.pss.2025.106034","url":null,"abstract":"<div><div>Spectral parameters of pyroxene estimated from the Moon Mineralogy Mapper (M³) hyperspectral data are used to delineate a total of twenty-two distinct compositional units in the southern quadrangle of the Moon (0°S to 30°S and 5°W to 30°W) covering four mare regions, namely, south-east Oceanus Procellarum, Mare Humorum, Mare Cognitum, and Mare Nubium. The compositional variation of pyroxenes and inferred crystallization temperatures indicate contrasting magmatic emplacement activity in the studied area. This finding is further strengthened by examining the variations in the FeO and TiO₂ content where units with titanium content (&gt;5.9 wt%) are associated with calcium content (&gt;30 wt%). The study further reveals two possible sources of magma, namely, a high titanium (Ti) high calcium pyroxene (HCP) magma source and a moderately titanium-rich high calcium pyroxene (HCP) magma source. Our crater size-frequency distribution (CSFD) study indicates that the volcanism prevailed in the study area from approximately 3.6 Ga to 0.73 Ga, peaking around ∼2.9 Ga to 1.5 Ga.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106034"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262390","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":"Potential bedrock exposures of Schrödinger impact melt sheet and/or polymict impact breccias within a crater floor fracture system and volcanic vent","authors":"David A. Kring ,&nbsp;Valentin T. Bickel ,&nbsp;Pascal Lee ,&nbsp;Amy L. Fagan ,&nbsp;Jennifer L. Heldmann ,&nbsp;Rick C. Elphic ,&nbsp;David J. Lawrence ,&nbsp;Timothy J. Parker ,&nbsp;Harrison H. Schmitt","doi":"10.1016/j.pss.2025.106063","DOIUrl":"10.1016/j.pss.2025.106063","url":null,"abstract":"<div><div>The Schrödinger impact basin provides significant geological targets for future exploration, including impact melts, multi-kilometer-long exposures of magmatic rocks from deep within the lunar crust, volcanic mare, pyroclastic ash deposits, potentially with mantle xenoliths, and a geophysical setting for examining the near-rim structure of the South Pole-Aitken mega-basin. Surveyor, Ranger, and Apollo programs confirmed that constant gardening of the lunar surface by impact cratering processes reduces the availability of outcrops, which are those key bedrock exposures that geologists on Earth use as the most reliable sources of information about planetary evolution. Lunar Reconnaissance Orbiter Camera (LROC) images of the lunar surface are providing data needed to identify bedrock exposures on the Moon, and tracked boulders leading to rock exposures, in locations suitable for future exploration. One such rocky exposure occurs within a volcanic vent within the Schrödinger impact basin. We consider six working hypotheses for its origin and conclude it likely represents a bedrock exposure of impact melt and/or impact breccia produced by the Schrödinger impact event or, alternatively, pristine lava rock associated with the vent's pyroclastic origin. While elsewhere in the basin those units are covered with regolith and younger volcanic deposits, the opening of a crater floor fracture and pyroclastic eruption of volcanic material cleared a vertical exposure through the impact or eruptive lithologies, which remain accessible for exploration today.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106063"},"PeriodicalIF":1.8,"publicationDate":"2025-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284617","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":"Geological history of Theia Mons, Beta Regio plume, Venus: Recognition of two main magmatic centers for flows, radiating dyke swarms and triple junction rifting","authors":"A.S. Shimolina ,&nbsp;R.E. Ernst ,&nbsp;H. El Bilali ,&nbsp;D.G. Malyshev ,&nbsp;V.E. Rozhin ,&nbsp;E.G. Antropova","doi":"10.1016/j.pss.2025.106050","DOIUrl":"10.1016/j.pss.2025.106050","url":null,"abstract":"<div><div>Theia Mons (centered at 23.4° N, 79.4° W) is the main volcanic center for the Beta Regio plume, of the Beta-Atla-Themis (BAT) region, Venus. Synthetic aperture radar data (SAR) and altimetry data from the 1989–1994 NASA Magellan mission were used to produce a geological map and history of Theia Mons, revealing two distinct magmatic centers (200 km apart), each the focus of basaltic lava flows, extensional lineaments (representing the surface expression of dyke swarms), and associated rift zones. The study area spans 88°W to 72°W, 16°45′N to 29°45′N, and mapping was at 1:500,000 scale. Our detailed mapping makes this area a prime target for the future Venus missions (orbital and lander), also given that Beta Regio is a strong candidate for ongoing volcanic activity.</div><div>Lava (basaltic) flow units (88 distinguished on the basis of variation in radar backscatter) belonging to Theia Mons volcano were combined into 19 Flow Groups and then into 3 Flow Packages. The lava flows appear to diverge from two distinct magmatic centers, labelled Center 1 (24.5°N, 78.1°W) and Center 2 (23.4° N, 79.4°W), with the older Center 1 being obscured by the volcanism of the younger Center 2. Center 1 consists of flows with low radar brightness and which extend to a maximum to 830 km from the center. Center 2 coincides with the currently preserved central caldera and consists of lava flows of low radar brightness with a maximum length of 620 km, followed by a second pulse of radar-bright flows that are less extensive and concentrated near the center.</div><div>About 10,000 extensional lineaments (grabens, fissures, and fractures) were mapped and grouped into 19 systems, of which 15 are interpreted to overlie dyke swarms: 2 radiating systems are associated with Centers 1 and 2, and 13 other systems belong to other (older and likely unrelated) magmatic centers in the region. A partial circumferential swarm may also be present, associated with Center 2.</div><div>Four other extensional lineaments sets are inferred to represent sets of normal faults associated with rift zones (Devana and Zverine, and additional rift zones). These rift zones exhibit two sets of ‘triple junction’ geometry, which are approximately also focussed on the same Centers 1 and 2, revealed by the lava flows and rift zones.</div><div>An underlying mantle plume is interpreted to be responsible for the dykes, flows and triple junction rifting. The cause of the shift between Centers 1 and 2 (200 km to SW) is unknown, but plausible mechanisms include a shift of the lithospheric plate above a stationary single plume, or a bending of the mantle plume (e.g. in a mantle wind) between timing of Center 1 and Center 2 activity.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106050"},"PeriodicalIF":1.8,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284621","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":"Low temperature fluorescence excitation and emission spectra of molecules relevant to Mars: Chlorobenzene, benzoic acid, phthalic acid, mellitic acid, and benzene in water ice solutions at temperatures between 78 K and 273 K","authors":"Suresh Sunuwar,&nbsp;Carlos E. Manzanares","doi":"10.1016/j.pss.2025.106054","DOIUrl":"10.1016/j.pss.2025.106054","url":null,"abstract":"<div><div>The discovery of chlorobenzene detected in soil samples obtained in Mars has been the subject of several interpretations. The original sample was subjected to pyrolysis before the gas chromatography-mass spectrometry (GC-MS) separation and identification with the Sample Analysis at Mars (SAM) instrument on the Curiosity rover. It is believed that chlorobenzene detected at concentrations above the background level of the instrument was a product of other organic molecules reacting with perchlorates of the Martian soil. Mars surface temperatures may reach a high of about 293 K at noon, at the equator, and a low of about 120 K at the poles. In this paper, characteristic fluorescence excitation and emission spectra are presented for chlorobenzene and the suggested precursor molecules: benzoic acid, phthalic acid, and mellitic acid in transparent hexagonal water ice solutions at temperatures between 273 K and 78 K. In addition, the liquid solution spectra at 292 K. Spectra of benzene in water ice solutions have also been included. The experimental results presented in this paper are to be compared with fluorescence experiments of Mars missions that will explore the polar regions and other regions where water ice is expected to be found. Limits of detection at part per billion by mass (ng/g) concentrations at room temperature are discussed based on our results and the literature. The application of fluorescence for low temperature studies of Mars samples is also discussed with a proposed miniature instrument with a laser source to increase the sensitivity of the detection and could be used for solid or liquid samples.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106054"},"PeriodicalIF":1.8,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284560","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}