Planetary and Space Science最新文献

{"title":"Numerical experiments on the hydrodynamic structure of a barchan dune constrained by dense atmospheres: Comparative applications to Venus and Titan","authors":"Xiaosi Zhou","doi":"10.1016/j.pss.2025.106115","DOIUrl":"10.1016/j.pss.2025.106115","url":null,"abstract":"<div><div>Venus and Titan, two very different terrestrial bodies in the solar system possessing extremely hot and extremely cold near-surface dense atmospheres, respectively, have been identified as having surface dune distributions associated with aeolian sand transport. Previous studies on planetary dunes have rarely involved a detailed investigation of flow behavior over dunes under such extreme environmental conditions. This study takes the highly migratory elementary barchan dune as the research object, and aiming at the realistic thermophysical environment of the wind field near the surfaces of Venus and Titan, a computational fluid dynamics model of the turbulent boundary layer on the surface that considers the real gas effect and planetary gravity constraints was constructed to carry out numerical experiments and comparative analysis of the hydrodynamic behavior of sand dunes induced by different planetary atmospheric environments. The predicted results show that there are notable differences in the leeward secondary flow structures of the barchan dunes induced by the real gas flows of Venus and Titan. Under the conditions of a 0-km elevation and the same incident flow speed, the flow reattachment length of the Venusian dune is slightly smaller than that of Titan's dune. This may be caused by differences in the thermo-hydrodynamics of planetary atmospheric fluids and differences in the turbulent flow represented by the flow Reynolds number. In essence, for Venusian dunes with high Reynolds number turbulence, the kinematic viscosity, as the only variable parameter, has no significant impact on the flow reattachment length. At the same wind intensity conforming to the in-situ data, for both Venus and Titan, the dune areas where the wind can cause fine sand of the same size to take off and subsequently be eroded tend to be located on the crest of the dune. The maximum dimensionless friction velocity, which is used to characterize the erosion intensity, decreases linearly with increasing elevation on Venus. This indirectly clarifies the previous argument about the relationship between planetary atmospheric density and aeolian geomorphology scales in a new light. The quantitative comparisons of the eroded extent and intensity on dune surfaces suggest that the induced effect of the atmospheric environment on Titan at 0 km is the closest to that on Venus at 11 km. This research can provide inspiration and a theoretical reference for the study of comparative planetology in the field of aeolian geomorphology.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"261 ","pages":"Article 106115"},"PeriodicalIF":1.8,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143816979","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":"Pre-perihelion observations of the carbon-depleted comet C/2023 A3 (Tsuchinshan-ATLAS). Insights into CN production and molecular upper limits","authors":"Pamela Cambianica ,&nbsp;Giovanni Munaretto ,&nbsp;Gabriele Cremonese ,&nbsp;Alessandra Mura ,&nbsp;Fiorangela La Forgia ,&nbsp;Luca Bizzocchi ,&nbsp;Monica Lazzarin ,&nbsp;Cristina Puzzarini ,&nbsp;Mattia Melosso ,&nbsp;Vania Lorenzi ,&nbsp;Walter Boschin","doi":"10.1016/j.pss.2025.106102","DOIUrl":"10.1016/j.pss.2025.106102","url":null,"abstract":"&lt;div&gt;&lt;div&gt;The study of cometary molecular emissions provides crucial insights into the primordial composition of the Solar System and the physical and chemical processes shaping these icy bodies. Comets, as remnants of the early Solar System, serve as natural archives of volatile compounds that offer a glimpse into the conditions of the protoplanetary disk. In this work, we analyze an optical pre-perihelion spectrum of comet C/2023 A3 (Tsuchinshan-ATLAS), obtained using the DOLORES spectrograph at the Telescopio Nazionale Galileo (TNG) on May 1, 2024. The cometary spectrum was reduced using standard procedures implemented in the IRAF software package. To characterize the volatile inventory of comet C/2023 A3, we derived the production rate of CN, the only detectable molecular emission, and calculated upper limits for undetected species, including C&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;, C&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;3&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;, and NH&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;. These constraints were obtained by analyzing the noise level in continuum regions and integrating theoretical line profiles, accounting for instrumental resolution and observational conditions. We calculated a CN production rate of (3.89&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;±&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;21&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;)&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;25&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; molec/s. Despite significant dust contamination, which likely obscures weaker molecular emission lines typically associated with cometary activity, we derived upper limits for the production rates of key volatile species: Q&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;C&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;3&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;&lt;&lt;/mo&gt;&lt;mn&gt;3&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;12&lt;/mn&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;24&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; molec/s, Q&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;C&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;&lt;&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;30&lt;/mn&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;25&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; molec/s, and Q&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;N&lt;/mi&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;H&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;&lt;&lt;/mo&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;79&lt;/mn&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;25&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; molec/s, respectively. We also determined the &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;A&lt;/mi&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mi&gt;ρ&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; parameter, obtaining a value of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mn&gt;4329&lt;/mn&gt;&lt;mo&gt;±&lt;/mo&gt;&lt;mn&gt;56&lt;/mn&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; cm, which confirms the high dust production rate previously reported for this comet. The logarithmic ratio of production rates, &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;log&lt;/mo&gt;&lt;mfenced&gt;&lt;mrow&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"261 ","pages":"Article 106102"},"PeriodicalIF":1.8,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143785187","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":"Photothermal spectroscopy for planetary sciences: Mid-IR absorption made easy","authors":"Christopher Cox ,&nbsp;Jakob Haynes ,&nbsp;Christopher Duffey ,&nbsp;Christopher Bennett ,&nbsp;Julie Brisset","doi":"10.1016/j.pss.2025.106101","DOIUrl":"10.1016/j.pss.2025.106101","url":null,"abstract":"<div><div>The understanding of the formation and evolution of the solar system still has many unanswered questions. Formation of solids in the solar system, mineral and organic mixing, and planetary body creation are all topics of interest to the community. Studying these phenomena is often performed through observations, remote sensing, and in-situ analysis, but there are limitations to the methods. Limitations such as IR diffraction limits, spatial resolution issues, and spectral resolution issues can prevent detection of organics, detection and identification of cellular structures, and the disentangling of granular mixtures. Optical-PhotoThermal InfraRed (O-PTIR) spectroscopy is a relatively new method of spectroscopy currently used in fields other than planetary sciences. O-PTIR is a non-destructive, highly repeatable, and fast form of measurement capable of reducing these limitations. Using a dual laser system with an IR source tuned to the mid-IR wavelength we performed laboratory O-PTIR measurements to compare O-PTIR data to existing IR absorption data and laboratory FTIR measurements for planetary materials. We do this for the purpose of introducing O-PTIR to the planetary science community. The technique featured here would serve to better measurements of planetary bodies during in-situ analysis. This is due to the technique’s ability to match absorption features in the mid-IR while performing non-contact analysis at a sub-micron level. We find that for the materials discussed in this work, O-PTIR was capable of identifying materials when utilizing known features and peaks of comparable absorption spectra.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"261 ","pages":"Article 106101"},"PeriodicalIF":1.8,"publicationDate":"2025-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143800554","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":"New empirical phase function of the lunar surface brightness derived from analysis of LROC WAC data as a tool for remote sensing of the Moon","authors":"Viktor Korokhin ,&nbsp;Yuri Velikodsky ,&nbsp;Yehor Surkov ,&nbsp;Sergey Velichko","doi":"10.1016/j.pss.2025.106099","DOIUrl":"10.1016/j.pss.2025.106099","url":null,"abstract":"<div><div>A comparison of various expressions of phase function of brightness of the lunar surface was carried out and recommendations were given for their use for the reduction of photometric observations and solving the problems of remote sensing of the lunar surface. A new empirical phase <em>χ</em>-function derived from analysis of LROC WAC data is proposed. It has only two free parameters, but it allows for qualitative approximation of phase curves of the brightness for morphological formations of different nature both for Maria and Highlands, thus it is useful for photometric reduction of observation data. Parameter <em>χ</em> of this function does not depend on albedo (wavelength) and can serve as an assessment of the structural characteristics of the lunar surface, which is useful for solving the problems of remote sensing of the lunar surface. Parameter <em>χ</em> of this function also can serve as an effective tool for detecting new photometric anomalies on the surface of the Moon.</div><div>The results of the work are applicable for remote sensing of any atmosphereless surfaces of with complex topography.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106099"},"PeriodicalIF":1.8,"publicationDate":"2025-03-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143706289","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":"Opposition effect of M-type asteroids","authors":"I.G. Slyusarev ,&nbsp;V.G. Shevchenko ,&nbsp;I.N. Belskaya ,&nbsp;Yu N. Krugly ,&nbsp;V.G. Chiorny ,&nbsp;O.I. Mikhalchenko ,&nbsp;R. Ya. Inasaridze ,&nbsp;V.V. Ayvaczian ,&nbsp;V. Zhuzhunadze ,&nbsp;I.V. Reva ,&nbsp;Ch T. Omarov ,&nbsp;T. Kwiatkowski ,&nbsp;D. Oszkiewicz ,&nbsp;V. Troianskyi ,&nbsp;B.A. Skiff ,&nbsp;O. Maryeva ,&nbsp;S. Karpov ,&nbsp;Z. Donchev","doi":"10.1016/j.pss.2025.106103","DOIUrl":"10.1016/j.pss.2025.106103","url":null,"abstract":"<div><div>We present results of the observational program dedicated to search for possible diversity in opposition effect behavior of M-type asteroids. New photometric BVR observations were obtained for 10 asteroids, (325) Heidelberga, (382) Dodona, (558) Carmen, (639) Latona, (758) Mancunia, (789) Lena, (1046) Edwin, (1352) Wawel, (2582) Harimaya-Bashi, and (5615) Iskander. Five of these asteroids have diameters in the range from 5 to 40 km. For all of observed asteroids, we obtained lightcurves and magnitude-phase curves in a wide range of phase angles. We determined values of rotation periods and absolute magnitudes of these asteroids. With our new data, we doubled the number of M-type asteroids with measured opposition effect and for the first time observed opposition effect of M-type asteroids less than 40 km in diameter. We found that three asteroids, (558) Carmen, (789) Lena and (5615) Iskander, exhibit lower values of opposition effect compared to other measured M- and S-type asteroids but the slope of the linear part of the phase curve is typical for moderate-albedo surfaces. A possible explanation of their lower opposition effect is an assumption of a higher metal content on their surfaces as compared to other asteroids.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106103"},"PeriodicalIF":1.8,"publicationDate":"2025-03-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143696043","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":"Diurnal temperature cycle models and performances on Martian surface using in-situ and satellite data","authors":"Yu Wang ,&nbsp;Shuanggen Jin","doi":"10.1016/j.pss.2025.106100","DOIUrl":"10.1016/j.pss.2025.106100","url":null,"abstract":"<div><div>Martian surface temperature and its diurnal variations play a key role in studying Mars land-atmosphere interactions. However, accurate Diurnal Temperature Cycle (DTC) models on Martian surface are presently absent or have large uncertainties. This study aims to construct semi-empirical DTC models of the Martian surface and address this gap by assessing their performances. Utilizing in-situ data collected by the Viking 1, Insight, Perseverance, and Curiosity rovers, we assess the performances of these DTC models by examining overall accuracy, daily precision, error rates across various hours, and effectiveness during different Martian seasons. The parameters of the models gain insights into the seasonal variations of surface temperature on Mars. Additionally, we conduct a focused analysis on the parameter-reduction approaches (PRAs) to assess the potential suitability of DTC models with the constraints of limited satellite observations available for Mars. Results indicate that the DTC models can effectively capture the diurnal surface temperature variations on Mars, with an overall error ranging from 0.74 to 2.28 K. Among the DTC models, the DMT24 model developed in this study shows the superior performance and can reproduce the slow and smooth increase around sunrise and maintain accuracy during nighttime periods. The DTC models can well capture the diurnal surface temperature cycle on Mars using limited satellite data based on suitable PRAs. This study offers valuable references for utilizing global DTC models on Mars.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106100"},"PeriodicalIF":1.8,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143696044","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":"Key structural characteristics of porous layers in diffusion modelling: A study on polydispersity, shape, and hierarchy","authors":"Volodymyr Reshetnyk ,&nbsp;Igor Luk’yanyk ,&nbsp;Yuri Skorov ,&nbsp;Yevgen Grynko ,&nbsp;Wolfgang Macher ,&nbsp;Christian Schuckart ,&nbsp;Yuhui Zhao ,&nbsp;Jürgen Blum","doi":"10.1016/j.pss.2025.106078","DOIUrl":"10.1016/j.pss.2025.106078","url":null,"abstract":"<div><div>In this study, we explored various open-source models for generating porous media. These models enabled us to examine different types of porous beds, including layers of polydisperse spheres with various size distributions, layers of porous aggregates – either fragments of parent porous layers or those formed during the agglomeration of polydisperse spheres – and layers of non-spherical particles with both regular and random shapes. Through extensive simulations, we derived estimates for the averaged structural characteristics of the model layers. These estimates will be utilized in macroscopic models to study heat diffusion and the sublimation of products in the near-surface layer of a cometary nucleus. Our findings revealed significant differences between the obtained estimates and those previously made for layers of monodisperse spheres, underscoring the importance of this research. We also compared numerical results with theoretical formulas for layers of monodisperse spheres.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106078"},"PeriodicalIF":1.8,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143679681","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":"Astrometric performance of the five major uranian satellites using a narrow-band Methane filter","authors":"X.Q. Fang ,&nbsp;Q.Y. Peng ,&nbsp;X. Lu ,&nbsp;B.F. Guo","doi":"10.1016/j.pss.2025.106085","DOIUrl":"10.1016/j.pss.2025.106085","url":null,"abstract":"<div><div>During ground-based observations of satellites near a bright planet, the satellite images are often affected by the planet’s halo, introducing significant uncertainty in their astrometric positions. To address this issue, we employed a narrow-band methane filter for observations of the five major Uranian satellites, which makes them easily discernible on CCD frames without requiring halo removal procedures. We systematically evaluated the astrometric performance of this <em>Methane</em> filter and compared it to that of the commonly used <em>Clear</em> and <em>Cousins-I</em> filters. Totally, the positional precision for most of the four brightest satellites is approximately 30 mas in both right ascension and declination, comparable to the <em>Cousins-I</em> filter and superior to the <em>Clear</em> filter. On the other hand, the faint satellite Miranda achieves a precision of better than 80 mas after image stacking in the methane band images. Based on our experiments, we recommend using the <em>Methane</em> filter for observing objects with an apparent visual magnitude brighter than 15, as it offers a sufficient signal-to-noise ratio (SNR) of approximately 55 within a reasonable exposure time of 200 s using a 0.8 m telescope.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106085"},"PeriodicalIF":1.8,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143644833","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":"Effective feature matching of high-resolution planetary orbiter images based on optimized image partitioning and rapid local correspondence","authors":"Lin Xue ,&nbsp;Zhen Ye ,&nbsp;Dayong Liu ,&nbsp;Shijie Liu ,&nbsp;Rong Huang ,&nbsp;Huan Xie ,&nbsp;Yongjiu Feng ,&nbsp;Beibei Guo ,&nbsp;Yusheng Xu ,&nbsp;Xiaohua Tong","doi":"10.1016/j.pss.2025.106091","DOIUrl":"10.1016/j.pss.2025.106091","url":null,"abstract":"<div><div>Feature matching of high-resolution planetary orbiter images (HRPOIs) plays a significant role in photogrammetric mapping and three-dimensional modeling, which is particularly challenging due to their narrow fields of view, similar surface textures, and large sizes. Neither directly using matching methods nor combining them with traditional strategies can fully overcome the matching challenges posed by HRPOIs. In this study, a feature matching scheme specifically designed for HRPOIs is proposed, which integrates an optimized image partitioning method for overlapping areas and establishes rapid local correspondence between image blocks. A row-to-column grid partitioning method is developed to ensure the range of the partitioned image blocks better align with the boundaries of the complex overlapping areas. Subsequently, the relative positional relationships of the extreme coordinate points in the row direction within the overlapping areas of image pairs are determined to rapidly establish local correspondence between the partitioned images, providing local geometric constraints and avoiding interference caused by redundant features. Moreover, a multilevel efficiency optimization strategy, which combines Graphics Processing Unit (GPU) acceleration with distributed parallelism to enhance the matching efficiency, is designed. Experiments on data derived from the Lunar Reconnaissance Orbiter Narrow Angle Camera (LRO NAC) and Mars Reconnaissance Orbiter Context Camera (MRO CTX) were conducted to validate the feasibility and reliability. The experimental results demonstrate that the proposed scheme effectively overcomes the challenges faced when matching HRPOIs, outperforming several mainstream photogrammetric software in terms of both matching accuracy and efficiency.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106091"},"PeriodicalIF":1.8,"publicationDate":"2025-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143679680","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":"Robust automatic crater detection at all latitudes on Mars with deep-learning","authors":"L. Martinez ,&nbsp;F. Andrieu ,&nbsp;F. Schmidt ,&nbsp;H. Talbot ,&nbsp;M.S. Bentley","doi":"10.1016/j.pss.2025.106053","DOIUrl":"10.1016/j.pss.2025.106053","url":null,"abstract":"<div><div>Understanding the distribution and characteristics of impact craters on planetary surfaces is essential for unraveling geological processes and the evolution of celestial bodies. Several machine learning and AI-based approaches have been proposed to detect craters on planetary surface images automatically. However, designing a robust tool for an entire complex planet such as Mars, is still an open problem. This article presents a novel approach using the Faster Region-based Convolutional Neural Network (Faster R-CNN) for such a detection. The proposed method involves the pre-processing, training and crater detection steps, which are especially designed for robustness regarding latitude and complex geomorphological features. The objectives of this studies are to (i) be robust at all latitudes and (ii) for <span><math><mrow><mo>≥</mo><mn>1</mn></mrow></math></span> km diameter crater sizes. (iii) To propose an open-source and re-usable algorithm that (iv) only needs an image to run. Extensive experiments on high-resolution planetary imagery demonstrate excellent performances with an average precision <span><math><mrow><msub><mrow><mtext>AP</mtext></mrow><mrow><mn>50</mn></mrow></msub><mo>&gt;</mo><mn>0</mn><mo>.</mo><mn>82</mn></mrow></math></span> with an intersection over union criterion <span><math><mrow><mtext>IoU</mtext><mo>≥</mo><mn>0</mn><mo>.</mo><mn>5</mn></mrow></math></span>, irrespective of crater scale. For mid and high latitudes (higher than 48°north and south), performance decreases down to <span><math><mrow><msub><mrow><mtext>AP</mtext></mrow><mrow><mn>50</mn></mrow></msub><mo>∼</mo><mn>0</mn><mo>.</mo><mn>7</mn></mrow></math></span>, which is still better than the current state of the art. Loss of performance is mostly due to strong shadowing effects. Our results also highlight the versatility and potential of our robust model for automating the analysis of craters across different celestial bodies. The automated crater detection tool presented in this article is publicly available as open-source and holds great promise for future scientific research of space exploration missions.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106053"},"PeriodicalIF":1.8,"publicationDate":"2025-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143644835","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}