Planetary and Space Science最新文献

{"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}

{"title":"Three-dimensional simulation of surface charging in meteorite craters on rotating asteroids","authors":"Zhiying Song,&nbsp;Zhigui Liu,&nbsp;Ronghui Quan","doi":"10.1016/j.pss.2025.106089","DOIUrl":"10.1016/j.pss.2025.106089","url":null,"abstract":"<div><div>Meteorite craters on the asteroid surface obstruct the horizontal flow of solar wind, forming a plasma wake that modulates the particle fluxes and the electrostatic environment far downstream. In this study, the surface charging properties of asteroids with nontrivial terrain are simulated on the basis of the neural network and the finite element method. Key factors such as the location, size and depth-to-width ratio of craters are all considered. Under normal conditions, as the latitude of the crater increases, the potential variation at its floor during a rotation gradually becomes smoother, finally stabilizing around −27.5 V with minor fluctuations when the crater approaches the poles. Because of the diverging motions of electrons and the less deflected trajectories of ions, near the terminator, the surface potential variation within craters with low depth-to-width ratios primarily depends on ion density, which decreases with increasing depth. In contrast, for craters with a depth-to-width ratio greater than 0.5, the potential differences at the crater floor arise mainly from the electron distribution. While the surface potential appears indifferent to changes in crater size, only during solar storms, the floor of large-scale craters, such as those with a diameter of 800 m, perform a 26.78 V decrease in potential compared to small craters of 50 m. Both studies of localized plasma flow field and the surface charging phenomenon of asteroids have substantial influence on the future safe landing and exploration missions.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"260 ","pages":"Article 106089"},"PeriodicalIF":1.8,"publicationDate":"2025-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143627907","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":"Three dimensional (3-D) density structures for the lunar mascons beneath impact basins and its implication for the evolution of the moon","authors":"Jianguo Yan ,&nbsp;Brave Manda ,&nbsp;Feng Liang ,&nbsp;Chikondi Chisenga ,&nbsp;Zhiyong Xiao ,&nbsp;Qingyun Deng","doi":"10.1016/j.pss.2025.106090","DOIUrl":"10.1016/j.pss.2025.106090","url":null,"abstract":"<div><div>Lunar mascons are thought to be caused by mantle uplift. We study lunar mascons to reveal their high-resolution 3D density structure based on the depth-weighting gravity inversion method. The inversion results show that mascons exhibit annular density anomalies, but the roots of mascons on the lunar nearside are shallower than those at the farside, which is consistent with the thicker crust at the lunar farside. Inner density heterogeneity for mascons is also observed in the density model, indicating evidence of the possible vertical and horizontal isostatic readjustment. Based on the density models, we suggest that the crustal asymmetry on the Moon observed in lunar basin thickness, size, and diameter is partly caused by mascon density heterogeneity located in the mantle that promoted mantle uplift after impact cratering, as observed in the recovered density models for lunar mascon.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"259 ","pages":"Article 106090"},"PeriodicalIF":1.8,"publicationDate":"2025-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143619202","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":"Relaxation probe measurement in the Earth's and Titan's atmospheres: Effect of shadow","authors":"John D. de Boer ,&nbsp;R. Godard ,&nbsp;José J. López-Moreno ,&nbsp;Gregorio J. Molina-Cuberos","doi":"10.1016/j.pss.2025.106088","DOIUrl":"10.1016/j.pss.2025.106088","url":null,"abstract":"<div><div>In this work, we investigate the shadowing effect of the boom and the gondola on electrical conductivity measurement in the stratosphere using a Relaxation Probe (RP). By taking the examples of the terrestrial flight for the Huygens experiment and the Huygens mission to Titan, our numerical simulations demonstrate that this effect should be taken into account, particularly for the resistance of the electrode-ionized medium during both the apogee and descent of a balloon. The fact that a signal seems a perfect exponential does not allow one to accept the hypothesis of a measurement at face value, and a correction factor should be applied. Our numerical simulations show that the resistance and the capacitance are almost constant, independent of the potential of the electrode. This makes the correction of the data an easy task. This analysis was carried out using finite element methods to model a complex electrode-boom-gondola geometry. In our model, the potential around the electrode-boom-gondola system is described by a Laplace equation, and this corresponds well to the stratospheric environment. We shall emphasize the crucial importance of estimating the floating potential of the gondola during a flight from the relaxation data of the potential. From our numerical simulations, it appears that the resistance may be too high by a factor 1.72, depending of course on the length of the boom. Also, the measurement of the positive ions by the RP for the Huygens mission around Titan does not seem too reliable. In this case, we found a heavy shadowing effect of the gondola. We hope that this work will aid in the optimal design of future planetary missions, taking into account the length of boom and, given the constraints of a mission, whether the boom should be an insulator, or a conducting body.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"259 ","pages":"Article 106088"},"PeriodicalIF":1.8,"publicationDate":"2025-03-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143570551","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An energy balance climate model for Mars represented by 4002 Goldberg polyhedrals with applications to ground ice re-distribution driven by obliquity cycles","authors":"Robert Olszewski ,&nbsp;Piotr Pałka ,&nbsp;Agnieszka Wendland ,&nbsp;Alison F.C. Bridger ,&nbsp;Melinda A. Kahre ,&nbsp;Christopher P. McKay","doi":"10.1016/j.pss.2025.106077","DOIUrl":"10.1016/j.pss.2025.106077","url":null,"abstract":"<div><div>We have developed a surface energy balance model for Mars based on representing the surface of Mars with a Goldberg polyhedral of 4002 cells. The approach using discretization of space with Goldberg polygons made it possible not only to obtain homogeneous spatial resolution but also the absence of a singularity at the poles in the model. In addition to the radiation terms, the surface energy balance includes CO₂ condensation and evaporation, the diffusive exchange of heat between cells, heat exchange with the subsurface, and a representation of the large-scale transport of heat from the equator to pole. We validate the model by comparing model results to the Viking lander temperature and pressure data. The model results are within 10% in both temperature and pressure compared to both Viking 1 and Viking 2 landers. We also compare to current Mars GCMs. Our baseline model has a total exchangeable CO₂ mass equivalent to 700 Pa and a mean annual surface temperature of 215.9 K. We use the baseline model to investigate the effects of changes in obliquity on climate. With all other model parameters held constant we find that as the obliquity increases above ∼30° the mean annual vapor density of ground ice at the poles becomes greater than at the equator implying a net transfer of water from pole to equator. We also find there is 95% consistency with the MCD model in CO₂ ice formation. The Mars polyhedral model has high spatial resolution but is still computationally efficient and can be used to simulate a variety of processes on Mars, at present or in past and future epochs.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"259 ","pages":"Article 106077"},"PeriodicalIF":1.8,"publicationDate":"2025-03-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143592209","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":"Production of carbon samples with extreme physical conditions using intense heavy ion beams at the facility for antiprotons and ion research: Application to planetary physics research","authors":"N.A. Tahir ,&nbsp;V. Bagnoud ,&nbsp;P. Neumayer ,&nbsp;A.R. Piriz ,&nbsp;S.A. Piriz","doi":"10.1016/j.pss.2025.106074","DOIUrl":"10.1016/j.pss.2025.106074","url":null,"abstract":"<div><div>The possibility of existence of carbon-rich-planets makes it important to study High Energy States of carbon in order to understand the internal structure of such planets. In this paper, we present two-dimensional hydrodynamic simulations of a low-entropy compression of a carbon sample that is enclosed in a high-Z cylindrical shell that is driven by a high intensity uranium beam. The considered beam parameters are the ones that will be available at the accelerator facility, named, FAIR, at Darmstadt. This study has shown that the carbon sample can be compressed to 2 to 3 times solid density and ultra-high pressures are achieved. The temperature, on the other hand, remains relatively low. These are the typical physical conditions that are expected to exist in the planetary interiors. An experimental study of the thermophysical and transport properties of such samples will significantly improve our knowledge about formation and evolution of different type of planets.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"259 ","pages":"Article 106074"},"PeriodicalIF":1.8,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143519277","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":"Maximizing the velocity deflection of asteroid Didymos using the Whale Optimization Algorithm","authors":"Iman Shafieenejad","doi":"10.1016/j.pss.2025.106075","DOIUrl":"10.1016/j.pss.2025.106075","url":null,"abstract":"<div><div>This study aims to optimize the velocity change of the Didymos asteroid using the Whale Optimization Algorithm (WOA). The deflection of asteroids that pose significant threats to Earth is a crucial aspect of upcoming space missions. In this research, a spacecraft is attached to the Didymos asteroid, utilizing its gravitational force as a perturbation to modify the asteroid's trajectory. The transfer of kinetic energy from the spacecraft to the asteroid induces a change in velocity (ΔV). The findings indicate that the most substantial impact on velocity occurs in the radial direction, showing divergent oscillatory behavior. The results suggest that the optimal point for significant velocity change is located shortly after the perihelion. At this point, WOA achieves the maximum velocity change. Additionally, the stability of the asteroid's deflection is investigated due to the nonlinear characteristics of the orbital motion equations. The optimal velocity change is identified as <span><math><mrow><mo>Δ</mo><msub><mi>V</mi><mrow><mi>t</mi><mi>o</mi><mi>t</mi><mi>a</mi><mi>l</mi></mrow></msub><mo>=</mo><mn>2.5139</mn><mo>×</mo><mn>1</mn><msup><mn>0</mn><mrow><mo>−</mo><mn>7</mn></mrow></msup><mrow><mo>(</mo><mfrac><mrow><mi>k</mi><mi>m</mi></mrow><mi>s</mi></mfrac><mo>)</mo></mrow></mrow></math></span> at <span><math><mrow><mo>Δ</mo><mi>t</mi><mo>=</mo><mn>27.657</mn><mrow><mo>(</mo><mi>h</mi><mo>)</mo></mrow></mrow></math></span>, occurring after the perihelion at <span><math><mrow><msub><mrow><mi>t</mi><mrow><mo>(</mo><mi>h</mi><mo>)</mo></mrow></mrow><mrow><mo>Δ</mo><msub><mi>V</mi><mi>max</mi></msub></mrow></msub></mrow></math></span>. This study introduces a novel optimization approach for asteroid deflection, emphasizing the nonlinear dynamics of orbital motion.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"258 ","pages":"Article 106075"},"PeriodicalIF":1.8,"publicationDate":"2025-02-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143488289","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}