Icarus最新文献

{"title":"Microphysics of Europa’s surface using Galileo/NIMS","authors":"G. Cruz Mermy ,&nbsp;F. Schmidt ,&nbsp;F. Andrieu ,&nbsp;T. Cornet ,&nbsp;I. Belgacem","doi":"10.1016/j.icarus.2025.116739","DOIUrl":"10.1016/j.icarus.2025.116739","url":null,"abstract":"<div><div>Europa’s surface shows evidence of active resurfacing, which can be explained by endogenic processes. Apart from water ice, several chemical compounds have been proposed to account for the potential complex chemistry that could take place if a connection with the subsurface salty ocean were to occur. Previous spectroscopic studies that investigated the surface composition were limited by the number of compounds to consider due to the unavailability of laboratory measurements.</div><div>In a previous study (Cruz-Mermy et al., 2023), we tested for the first time the relevance of all possible combinations of 15 potential endmembers on a Galileo/NIMS observation of a dark lineament of the trailing anti-jovian hemisphere using realistic radiative transfer modeling and a robust Bayesian inference framework. This previous article was focused on the composition.</div><div>We report here on a follow-up exploratory study based on the same NIMS spectrum to determine robust microphysical characteristics of the surface. In the previous study, we considered an optimistic scenario corresponding to a 2% uncertainty in reflectance levels, equivalent to an SNR of 50. Based on this scenario, we showed that out of approximately 5,000 model combinations, only 174 provided a satisfactory fit to the selected NIMS spectrum. In this study, we focus on these best-fitting models and perform a statistical analysis on the estimated posterior distributions of the volume abundances and grain sizes for each of the 15 endmembers using all model combinations in which they are found. We show that despite the high number of potential good fits, a strong constraint on the volume abundance and grain size of the two mandatory compounds (sulfuric acid octahydrate – SAO – and water ice) can be drawn. We also show that these properties vary very little from one mixture to another, meaning we can successfully derive maps of these microphysical properties using a whole NIMS hyperspectral cube. Results on the hydrated sulfates and chlorinates show weaker but still sufficiently constrained volume abundances and grain sizes. Using a proxy such as the numerical abundance that links the volume abundance to the grain size to quantify the spectral contribution of the compounds allows a good representation of the surface for these compounds. However, it is still impossible to discriminate between these compounds by analyzing the microphysical properties obtained. The constraint on the estimated parameters would still allow us to derive the spatial distribution of these microphysical properties if the actual composition of the surface can be determined by other methods. Finally, we demonstrate that no constraint can be made about surface roughness with spectral analysis only.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116739"},"PeriodicalIF":3.0,"publicationDate":"2025-07-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144767118","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Tidal dissipation within Earth’s solidifying magma ocean: II. Atmospheric blanketing and its constraint on tidal heating","authors":"Jun Korenaga","doi":"10.1016/j.icarus.2025.116743","DOIUrl":"10.1016/j.icarus.2025.116743","url":null,"abstract":"<div><div>The early orbital evolution of the Earth–Moon system is strongly coupled with the thermal evolution of Earth’s magma ocean formed after the Moon-forming giant impact. The thermal budget of the magma ocean is dominated by the balance between tidal heating and the surface heat flux of the magma ocean. The former is effectively limited by the latter, because the magma ocean would stop cooling as soon as tidal heating is large enough to match the surface heat flux. One of the key factors controlling the magma ocean surface heat flux is the temperature difference at the surface, which is regulated by the thermal structure of the coexisting atmosphere. To evaluate the impact of tidal dissipation on the evolution of the Earth–Moon system, therefore, it becomes essential to understand how the cooling efficiency of Earth’s magma ocean is regulated by the thermal blanketing effect of the coexisting atmosphere, which is in turn affected by the degassing history of the magma ocean. In this work, we couple a comprehensive atmospheric model with a realistic mantle phase diagram to quantify how the surface heat flux from a magma ocean would change during the course of its solidification. Our results show that gray and nongray treatments result in about one order of magnitude difference in heat flux and that likely uncertainties in Earth’s volatile budget as well as degassing efficiency have a limited influence on magma ocean heat flux. Most importantly, the magnitude of tidal heating can be comparable to or even greater than magma ocean heat flux for a range of early Earth conditions, highlighting the fundamental role of atmospheric blanketing in the tidal evolution of the Earth–Moon system.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116743"},"PeriodicalIF":3.0,"publicationDate":"2025-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144739076","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Space weathering on Vesta: Ion bombardment induced changes on HEDs in visible and infrared reflectance","authors":"Stefano Rubino ,&nbsp;Francesca Zambon ,&nbsp;Rosario Brunetto ,&nbsp;Océane Barraud ,&nbsp;Sébastien Besse ,&nbsp;Ferenc Borondics ,&nbsp;Cristian Carli ,&nbsp;Jean-Philippe Combe ,&nbsp;Kerri Donaldson-Hanna ,&nbsp;Rachel Klima ,&nbsp;Cateline Lantz ,&nbsp;Giovanni Pratesi ,&nbsp;Katrin Stephan ,&nbsp;Federico Tosi","doi":"10.1016/j.icarus.2025.116755","DOIUrl":"10.1016/j.icarus.2025.116755","url":null,"abstract":"<div><div>The NASA/Dawn mission targeted <em>V</em>-type asteroid (4) Vesta between 2011 and 2012. The mission confirmed Vesta as the parent body of most of the HED meteorite family and led an extensive mapping of the surface's spectral properties. The well-pronounced different spectroscopic features of <em>V</em>esta suggest that this body has its own form of space weathering. In this work, we look for the optimal parameter space for distinguishing between fresh and weathered materials on Vesta and other V-type objects. We emulated the effects of the solar wind component of space weathering by performing ion bombardment experiments with 40 keV He⁺ on four HED meteorites. We then studied the spectral behavior of our artificially weathered samples, spanning from the visible to the mid-infrared range, using several spectral parameters. We observed that in the visible and near-IR range, the evolution of eight parameters – darkening of reflectance at 380–465-550 nm, decrease in band depth and band area of the 1-μm absorption feature, and reddening of three different spectral slopes - are enough to distinguish between differences in mineral composition and weathering state among our samples. In the mid-IR, we detected a consistent red shift in the position of the Reststrahlen feature, associated with sample weathering. These findings can provide support for the interpretation of remote sensing data from <em>V</em>-type objects, aiding in the assessment of mineralogical differences and the weathering state of surface materials.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116755"},"PeriodicalIF":3.0,"publicationDate":"2025-07-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144739088","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Database development and LIBS calibration for the LIBS-Raman Sensor for planetary exploration","authors":"E.R. Sawyers ,&nbsp;G. Lopez-Reyes ,&nbsp;A. Barlow ,&nbsp;M. Veneranda ,&nbsp;E.A. Lymer ,&nbsp;E.A. Cloutis ,&nbsp;J. Manrique ,&nbsp;B. Barrios ,&nbsp;S. Julve ,&nbsp;J. Freemantle ,&nbsp;M. Aznar ,&nbsp;M.G. Daly ,&nbsp;E.A. Lalla","doi":"10.1016/j.icarus.2025.116742","DOIUrl":"10.1016/j.icarus.2025.116742","url":null,"abstract":"<div><div>Laser-Induced Breakdown Spectroscopy (LIBS) has been a valuable technique in planetary exploration, providing rapid, in situ elemental analysis of extraterrestrial materials. The LIBS-Raman Sensor (LiRS), currently being evaluated for its capabilities for future planetary exploration missions at York University, integrates LIBS with complementary spectroscopic techniques to enhance geochemical and astrobiological investigations. To support the calibration and validation of this instrument, we have compiled a comprehensive database of well-characterized geological samples with known compositions, including carbonate, silicate, sulfate, and planetary simulant standards. These samples were analyzed under controlled conditions to create a robust machine learning-based elemental quantification dataset. Various statistical and regression models, including Gaussian Process Regression (GPR), Artificial Neural Networks (ANN), and Support Vector Machines (SVM), were evaluated for their predictive accuracy in determining compositions (as oxides). The results indicate that GPR consistently outperforms other methods for key planetary oxides such as SiO₂, Al₂O₃, and FeO<span><math><msub><mrow></mrow><mrow><mi>T</mi></mrow></msub></math></span>, while ANN and SVM offer strong performance for specific oxides like K₂O and MgO. This work demonstrates the potential of data-driven analytical techniques to improve LIBS-based geochemical analysis for future planetary missions. The developed database and models will aid in refining instrument calibration, improving spectral interpretation, and supporting ongoing planetary exploration efforts.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116742"},"PeriodicalIF":3.0,"publicationDate":"2025-07-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144757659","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Photodegradation of the biomarker L-histidine induced by edge sites of a clay mineral in the Martian harsh UV environment","authors":"Cristina García-Florentino ,&nbsp;Andrew Alberini ,&nbsp;Sole Biancalani ,&nbsp;Ophélie McIntosh ,&nbsp;John Brucato ,&nbsp;Juan Manuel Madariaga ,&nbsp;Maguy Jaber ,&nbsp;Teresa Fornaro","doi":"10.1016/j.icarus.2025.116757","DOIUrl":"10.1016/j.icarus.2025.116757","url":null,"abstract":"<div><div>Clay minerals are thought to play a crucial role in preserving organics on Mars due to their high surface area and expandable interlayers, ideal for adsorbing and intercalating organic molecules. Our study simulated the adsorption of L-histidine, an amino acid potentially diagnostic of life, on the clay mineral saponite, in a slightly acidic aqueous environment as possibly present on Mars during the Hesperian era, followed by a desiccation event and then high UV irradiation typical of the subsequent Amazonian era. For comparison, the same experiments were performed also at alkaline pH. X-Ray Diffraction and Infrared and Deep Ultraviolet Raman and fluorescence spectroscopies were used to characterize the mineral-molecule interactions, indicating that molecules are partly intercalated in the interlayers of saponite at acidic pH and partly co-precipitated with saponite at alkaline pH, while the remainder is adsorbed on lateral edges in both cases. Surprisingly, UV irradiation experiments revealed faster degradation of L-histidine when adsorbed on saponite compared to its pure form at both pHs, suggesting a photocatalytic behaviour of this nano-sized clay mineral, driven by active surface edge sites, despite potential shielding by interlayer sites for the part of L-histidine molecules intercalated in the interlayers at acidic pH. Degradation/alteration of L-histidine adsorbed on saponite occurs in a few hours under Martian UV flux, suggesting that photocatalysis induced by active surface edge sites of clays might have contributed to the depletion of organics in clays at the highly UV-irradiated surface of Mars on very short timescales.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116757"},"PeriodicalIF":2.5,"publicationDate":"2025-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144711010","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Where are the missing Kuiper Belt binaries?","authors":"Wladimir Lyra","doi":"10.1016/j.icarus.2025.116737","DOIUrl":"10.1016/j.icarus.2025.116737","url":null,"abstract":"<div><div>In this letter, we call attention to a gap in binaries in the Kuiper belt in the mass range between <span><math><mo>≈</mo></math></span>10¹⁹−10²⁰ kg, with a corresponding dearth in binaries between 4th and 5th absolute magnitude <span><math><mi>H</mi></math></span>. The low-mass end of the gap is consistent with the truncation of the cold classical population at 400 km, as suggested by the OSSOS survey, and predicted by simulations of planetesimal formation by streaming instability. The distribution of magnitudes for all KBOs is continuous, which means that many objects exist in the gap, but the binaries in this range have either been disrupted, or the companions are too close to the primary and/or too dim to be detected with the current generation of observational instruments. At the high-mass side of the gap, the objects have small satellites at small separations, and we find a trend that as mass decreases, the ratio of primary radius to secondary semimajor increases. If this trend continues into the gap, non-Keplerian effects should make mass determination more challenging.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116737"},"PeriodicalIF":3.0,"publicationDate":"2025-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144724169","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Rock suites of Endeavour crater, Mars: Comparing Perseverance Valley, Spirit of St. Louis, and Marathon Valley","authors":"Michael C. Bouchard,&nbsp;Bradley L. Jolliff","doi":"10.1016/j.icarus.2025.116752","DOIUrl":"10.1016/j.icarus.2025.116752","url":null,"abstract":"<div><div>Perseverance Valley is an erosional feature with the appearance of an eroded gully, located in the western wall of the Noachian aged Endeavour crater in Meridiani Planum, Mars. It is the most lithologically diverse location investigated by the Opportunity rover other than Cape York, where the rover first characterized the pre-, post-, and <em>syn</em>-depositional lithologies of Endeavour crater. We use hierarchical clustering and a similarity index combined with examination of Panoramic camera and Microscopic Imager images to classify these rock suites in Perseverance Valley, and contextualize them with comparison to rocks examined previously along the rim of Endeavour crater. The Perseverance Valley lithologies are classified into four rock suites, a clast-poor impact breccia that forms the “walls” of the valley, a competent basaltic outcrop of rocks that appear “blue” in false color Panoramic camera imagery, an outcrop of pitted rocks that has among the highest silica concentrations investigated by Opportunity, and a loose regolith mixture of martian soil, impact breccia, and local “blue” rocks that makes up the valley floor. Macro and micro textures indicate that the valley is currently being eroded by wind exiting the crater basin from west to east. Units that are offset both within and across Perseverance Valley indicate that the valley location and structure is likely influenced by a system of radial impact faults. Lithologies such as the co-located “blue” (in false color) and silica-rich pitted rocks, and observations of aqueous alteration such as “red” (in false color) zones, show similarities between Perseverance Valley and both Marathon Valley and the Spirit of St. Louis feature. We explore multiple working hypotheses to explain the formation mechanisms of Perseverance Valley, but can now say: the valley is likely structurally controlled including an ∼80 m vertical offset by a graben; the valley hosted local aqueous alteration; the floor material of the valley consists of mass-wasted local materials; and the current topographic expression was overprinted by modern aeolian erosion.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116752"},"PeriodicalIF":2.5,"publicationDate":"2025-07-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144703636","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Contribution of multi-ring basins to lunar production functions","authors":"Astrid Oetting ,&nbsp;Wajiha Iqbal ,&nbsp;Nico Schmedemann ,&nbsp;James W. Head ,&nbsp;Gregory Michael ,&nbsp;Harald Hiesinger ,&nbsp;Carolyn H. van der Bogert ,&nbsp;Thomas Heyer","doi":"10.1016/j.icarus.2025.116753","DOIUrl":"10.1016/j.icarus.2025.116753","url":null,"abstract":"<div><div>Crater size-frequency distribution (CSFD) measurements provide a valuable tool for dating surfaces on terrestrial planetary bodies. In order to derive an age from CSFD measurements, a production function (PF) is required to reflect the size-frequency distribution of craters being formed. However, the most commonly used PFs are only valid to crater diameters up to 300 km. An expansion of the PFs would be beneficial to improve the understanding of the early bombardment history of the Moon. However, there are two main issues affecting the interpretation of the CSFDs of large and multi-ring basins: the determination of a standard main basin rim for multi-ring basins and the low number of large basins. Previously, numerous attempts have been made to define the representative diameters for (multi-ring) basins, which appear in many lunar catalogs. The comparison of four such lunar crater catalogs revealed significant differences in defining basin boundaries and diameters. Therefore, we created a new crater catalog for lunar craters larger than 100 km based on topographic and gravity data and using a consistent definition for basin diameters. We found that on the highlands, the CSFD measurement has not reached equilibrium. Given that the number of empirically measured basins is limited, this investigation naturally must deal with low-number statistics. However, the available data for basins &gt;300 km still allow an empirical analysis to provide insights into this poorly understood part of the lunar PF. We find that the shape of the CSFD is consistent with the impactor size-frequency distribution (SFD) of the Main Asteroid Belt, suggesting an origin from the Main Asteroid Belt. The presence of an additional impactor population cannot be observed in our data, although we cannot exclude the possibility of a second population with a similar SFD. Using the highland CSFD measurement as a reference, we found interesting large discrepancies between the measured and the calculated number of craters and basins on the lunar mare. For instance, we measured 30 craters and basins ≥100 km on mare, but expected 79 using the PF of Neukum et al. (2001). In addition, we identified 9 basins ≥300 km on mare areas, but expected only 5 basins when applying the PF of Neukum et al. (2001).</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116753"},"PeriodicalIF":2.5,"publicationDate":"2025-07-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144711620","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Lithologies of Dimorphos revealed by boulder morphological classes","authors":"F. Tusberti ,&nbsp;M. Pajola ,&nbsp;L. Penasa ,&nbsp;A. Lucchetti ,&nbsp;M. Massironi ,&nbsp;G. Munaretto ,&nbsp;J. Beccarelli ,&nbsp;R. Pozzobon ,&nbsp;C. Rossi ,&nbsp;G. Poggiali ,&nbsp;N. Murdoch ,&nbsp;C.Q. Robin ,&nbsp;A. Duchene ,&nbsp;M. Amoroso ,&nbsp;I. Bertini ,&nbsp;J.R. Brucato ,&nbsp;A. Capannolo ,&nbsp;S. Caporali ,&nbsp;M. Ceresoli ,&nbsp;G. Cremonese ,&nbsp;L. Gomez Casajus","doi":"10.1016/j.icarus.2025.116744","DOIUrl":"10.1016/j.icarus.2025.116744","url":null,"abstract":"<div><div>The stony/Sq-type binary system (65803) Didymos consists of two rubble pile bodies, Didymos, the primary, and its moonlet Dimorphos. In 2022, the first planetary defense mission Double Asteroid Redirection Test (DART) reached Dimorphos and collected unprecedented high-resolution images of its surface. They revealed a variegated surface completely covered by stacked boulders and cobbles with different shapes and textures. Their morphological heterogeneity likely reflects the lithologies originally present within the Didymos and Dimorphos' parent body, before its fragmentation.</div><div>We present a lithologic study of Dimorphos' surface, based on a morphological analysis of its boulders. Our approach considers each boulder's 2D outline, perceived 3D shape, and surface texture characteristics. Based on these features, we identified two main morphological classes. A total of 178 boulders were classified as <em>Angular morphology</em> covering 38.5 % of the mapped area. This type is characterized by cohesive boulders with straight and angular outlines as well as sharp three-dimensional edges, which form well-defined sub-planar facets. Additionally, the texture of this kind of rocks show low-to-mid <em>Roughness</em> and the presence of lineations on some boulders. On the other hand, 210 boulders were categorized as <em>Hummocky</em> morphology, which covers 61.5 % of the area. Such morphology appears more friable and features boulders with rounded shaped and ragged and irregular 2D perimeter. Their 3D perceived shape appears as flat-to-curve, with rough and hummocky surface textures due to embedded clasts. We interpret the <em>Hummocky</em> morphology as breccia lithology. On the other hand, although Angular morphology can be associated with multiple potential lithologies, we interpret it as either an achondritic/igneous lithology or a highly metamorphosed chondritic lithology. The breccias are likely characteristic of the parent body's outer layers, actively involved in impact and sedimentary processes. Conversely, the lithologies associated with the <em>An</em> morphology should represent deeper regions of the plantesimal, possibly exhumed by impacts. All these results will be further complemented by data from the Hera mission, which will arrive at (65803) Didymos system at the end of 2026.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116744"},"PeriodicalIF":2.5,"publicationDate":"2025-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144711009","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"The model is the message: Lightweight convolutional autoencoders applied to noisy imaging data for planetary science and astrobiology","authors":"Caleb Scharf","doi":"10.1016/j.icarus.2025.116740","DOIUrl":"10.1016/j.icarus.2025.116740","url":null,"abstract":"<div><div>The application of convolutional autoencoder deep learning to imaging data for planetary science and astrobiological use is briefly reviewed and explored with a focus on the need to understand algorithmic rationale, process, and results when machine learning is utilized. Successful autoencoders train to build a model that captures the features of data in a dimensionally reduced form (the latent representation) that can then be used to recreate the original input. One application is the reconstruction of incomplete or noisy data. Here a baseline, lightweight convolutional autoencoder is used to examine the utility for planetary image reconstruction or inpainting in situations where there is destructive random noise (i.e., either luminance noise with zero returned data in some image pixels, or color noise with random additive levels across pixel channels). It is shown that, in certain use cases, multi-color image reconstruction can be usefully applied even with extensive random destructive noise with 90 % areal coverage and higher. This capability is discussed in the context of intentional masking to reduce data bandwidth, or situations with low-illumination levels and other factors that obscure image data (e.g., sensor degradation or atmospheric conditions). It is further suggested that for some scientific use cases the model latent space and representations have more utility than large raw imaging datasets.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"442 ","pages":"Article 116740"},"PeriodicalIF":3.0,"publicationDate":"2025-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144805815","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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}