Advances in Space Research最新文献

{"title":"Texture-based segmentation for sand and rock in Mars images","authors":"Omar Alkawi ,&nbsp;Rami Qahwaji ,&nbsp;Christina Smith ,&nbsp;Zied Mnasri","doi":"10.1016/j.asr.2025.05.034","DOIUrl":"10.1016/j.asr.2025.05.034","url":null,"abstract":"<div><div>The exploration of Martian’s surface is one of the most important aspects of understanding Martian environment. Investigating features such as sand dunes can provide valuable insights into Mars past environmental dynamics and geological history. However, self-driving in uncontrolled and unsupervised environments, like Mars, is a very challenging problem. To date, six Mars rovers have been successfully sent and operated on the surface, the latest of which is NASA’s Perseverance Rover and the next is planned to be ESA’s Rosalind Franklin rover. These cutting-edge spacecraft are driven by classical machine vision systems, which could cause some limitations to the safety, reliability, and productivity of these missions. This research aims to develop new technologies in Feature Extraction, Image Processing and Deep Learning for the identification of Mars Terrain to help future self-driving rovers navigate. Specifically, in this work, we focus on the identification of rocks and sands by utilising both linear (Gabor Filter), and nonlinear (Polynomial Bilateral Filter) feature extraction techniques. To combine the benefits of both filters we also investigate the effect of using image fusion technique. Our feature extraction response achieves promising results when integrated with deep learning methods with the highest accuracy achieved at 89.84 %. However, to improve the accuracy further, we analysed some of the images contributing to erroneous classifications. Most of these images feature low-contrast terrain, primarily due to dust or poor lighting conditions. A framework is introduced which includes a contrast investigation stage to determine the required level of image enhancement when processing the images. This resulted in an improved accuracy of 93.70 %. Finally, some suggestions for future improvements are included in this paper.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 3","pages":"Pages 1756-1773"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144579346","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"High latitude observation of the Forbush decrease during the May 2024 solar storms with muon and neutron detectors on Svalbard","authors":"F. Riggi ,&nbsp;L. Hertle ,&nbsp;M. Abbrescia ,&nbsp;C. Avanzini ,&nbsp;L. Baldini ,&nbsp;R. Baldini Ferroli ,&nbsp;G. Batignani ,&nbsp;M. Battaglieri ,&nbsp;S. Boi ,&nbsp;J. Boike ,&nbsp;E. Bossini ,&nbsp;F. Carnesecchi ,&nbsp;D. Cavazza ,&nbsp;C. Cicalò ,&nbsp;L. Cifarelli ,&nbsp;F. Coccetti ,&nbsp;E. Coccia ,&nbsp;A. Corvaglia ,&nbsp;D. De Gruttola ,&nbsp;S. De Pasquale ,&nbsp;O. Pinazza","doi":"10.1016/j.asr.2025.05.023","DOIUrl":"10.1016/j.asr.2025.05.023","url":null,"abstract":"<div><div>During the series of intense solar flares and coronal mass ejections, that occurred in May 2024, a remarkable Forbush decrease in the cosmic ray flux was observed on the Earth. While this event was observed by particle detectors around the world, the archipelago of Svalbard was heavily exposed to it due to the weak geomagnetic shielding in the polar region. In this study, an analysis of the Forbush decrease event was carried out with a unique combination of muon and neutron detectors on Svalbard: at Ny-Ålesund three scintillator-based muon telescopes of the Extreme Energy Events (EEE) project, 14 channels of a Bonner Sphere neutron Spectrometer (BSS), and thermal and epithermal neutron sensors used for hydrological monitoring; and, at Barentsburg, a high-energy neutron monitor operated by the Polar Geophysical Institute. Most sensors showed significant responses and correlation during the event. The observed relative magnitude of the Forbush decrease was found to depend on the detector’s energy sensitivity and was <span><math><mrow><mo>≈</mo><mn>9</mn><mspace></mspace><mo>%</mo></mrow></math></span> for thermal neutrons, <span><math><mrow><mo>≈</mo><mn>8</mn><mspace></mspace><mo>%</mo></mrow></math></span> for high-energy neutrons, and <span><math><mrow><mo>≈</mo><mn>3</mn><mspace></mspace><mo>%</mo></mrow></math></span> for muons. The uncertainty of these results strongly depends on factors like the count rate, which ranged from <span><math><mrow><msup><mrow><mn>10</mn></mrow><mrow><mn>1</mn></mrow></msup></mrow></math></span> to <span><math><mrow><msup><mrow><mn>10</mn></mrow><mrow><mn>5</mn></mrow></msup></mrow></math></span> cph and resulted in a low signal-to-noise ratio particularly for the BSS. These multi-particle and multi-energy observations provide an unprecendented view on the Earth’s exposure to cosmic rays during solar events.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 2","pages":"Pages 1225-1239"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144471578","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Operational insights and measurements of ChaSTE on the Chandrayaan 3 Vikram Lander","authors":"Nizy Mathew ,&nbsp;M. Ram Prabhu ,&nbsp;V. Aasik ,&nbsp;Fazil Mohammad ,&nbsp;Dinakar Prasad Vajja ,&nbsp;P.P. Pramod ,&nbsp;Kiran John Antony ,&nbsp;M. Satheesh Chandran ,&nbsp;K.P. Subhajayan ,&nbsp;V. Sathiyamoorthy","doi":"10.1016/j.asr.2025.05.024","DOIUrl":"10.1016/j.asr.2025.05.024","url":null,"abstract":"<div><div>Understanding the thermal properties of lunar regolith is crucial for accurately modelling heat transfer processes, evaluating the thermal behavior of lunar surface and subsurface, predicting volatile escape processes, and planning future exploration missions. Chandra’s Surface Thermophysical Experiment (ChaSTE) is a payload onboard Chandrayaan<!--> <!-->3 lander of Indian Space Research Organisation (ISRO), which measured temperature and thermal conductivity of lunar regolith by inserting a thermal probe into the regolith. This study details the timeline of ChaSTE activities on the lunar surface, the penetration operation of the ChaSTE probe into the regolith, and measurements of thermophysical properties such as packing density and thermal conductivity and temperature up to a depth of <span><math><mrow><mo>∼</mo></mrow></math></span>10<!--> <!-->cm at the landing location (69.37<!--> <!-->°<!--> <!-->S, 32.32<!--> <!-->°<!--> <!-->E) on the southern high-latitude region of the Moon. The mission life of ChaSTE was <span><math><mrow><mo>∼</mo></mrow></math></span>12 days during August<!--> <!-->–<!--> <!-->September, 2023. The measurements performed by ChaSTE are the first of their kind on the high-latitude lunar regolith.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 2","pages":"Pages 1196-1203"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144471622","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Unreleased sunspot records by Hacki in 1671 during the Maunder Minimum","authors":"V.M.S. Carrasco ,&nbsp;M. Jasiński ,&nbsp;J. Villalba-Álvarez ,&nbsp;A.J.P. Aparicio ,&nbsp;M.C. Gallego ,&nbsp;J.M. Vaquero","doi":"10.1016/j.asr.2025.05.037","DOIUrl":"10.1016/j.asr.2025.05.037","url":null,"abstract":"<div><div>The Maunder Minimum (1645–1715) was a period characterized by an abnormally low number of sunspots observed on the solar disc. This work focuses on solar activity in 1671, analyzing sunspot number data from a new historical documentary source: five letters exchanged between Hacki and Hevelius, which have been translated from Latin to English. These new records provide an independent confirmation of the sunspot groups observed in 1671, complementing previous works based on observations by other astronomers. Moreover, they highlight some corrections for future versions of the group number database. On the other hand, by compiling all sunspot data for 1671 published so far, we improve our knowledge of the solar activity level in that year. We obtained that the percentage of active days (days when sunspots were observed on the solar disc) was 21.3 %, although with a high uncertainty ranging between 6.3 % and 76.7 % considering days without any record as spotless or active days, respectively. Despite being one of the more active years in the Maunder Minimum, we conclude that the solar activity level in 1671 remains low in comparison to other periods of reduced solar activity, such as the Dalton Minimum. Thus, our study also impacts on the reconstruction of the solar cycle during the Maunder Minimum.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 2","pages":"Pages 1052-1059"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144471702","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Tracking Near-Earth Asteroids’ close approaches: 2023 DZ2, 2018 UY, and 2024 ON by the Southern Hemisphere Asteroid Research Consortium","authors":"Dorota Mieczkowska ,&nbsp;David Coward ,&nbsp;Arie Verveer ,&nbsp;John Kennewell ,&nbsp;Ed Kruzins","doi":"10.1016/j.asr.2025.05.036","DOIUrl":"10.1016/j.asr.2025.05.036","url":null,"abstract":"<div><div>We present an overview of the capabilities of the Australian collaboration for observing and characterising Near Earth Asteroids, with a focus on its geographic expansion to the West Coast of Australia. The West Coast node, supported by the University of Western Australia, uses the Zadko Observatory, equipped with several optical telescopes dedicated to Space Situational Awareness and Planetary Defence. We report observations of three selected asteroids during close approaches in the past two years: 2023 DZ2, 2018 UY, and 2024 ON. For 2023 DZ2, we demonstrate that despite highly variable photometric conditions, it is possible to extract the asteroid’s rotational signatures. Our analysis yields a rotational period of 6.2770 <span><math><mrow><mo>±</mo></mrow></math></span> 0.0450 min. The close approach of 2018 UY provided high-quality photometric data for a body with a previously unknown rotation, which we estimate to be 4.2759 <span><math><mrow><mo>±</mo></mrow></math></span> 0.3037 h for half of its full rotation. Our analysis reveals a significant periodic magnitude variation of (<span><math><mrow><mi>Δ</mi><mi>m</mi><mo>≈</mo><mn>1</mn></mrow></math></span>), indicating that the asteroid is highly elongated. Assuming a triaxial ellipsoid model, we estimate an upper limit for its elongation to be approximately 2.5 times longer than it is wide. Lastly, 2024 ON, likely a contact binary system, was discovered by NASA’s ATLAS system at Mauna Loa, Hawaii, on July 27, 2024. We present high-quality photometric data, potentially confirming the binary nature of this system with an estimated half-rotation period of 2.9789  <span><math><mrow><mo>±</mo></mrow></math></span>  0.1363 h.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 2","pages":"Pages 1163-1171"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144471620","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Stochastic properties of GNSS height time series caused by aperiodic part of environmental loading deformations: Case study in Beijing and its surrounding areas","authors":"Yifang Ma ,&nbsp;Yilin Yang ,&nbsp;Xiaohui Zhou ,&nbsp;Leyin Hu ,&nbsp;Wei Liu","doi":"10.1016/j.asr.2025.05.029","DOIUrl":"10.1016/j.asr.2025.05.029","url":null,"abstract":"<div><div>The comprehensive understanding of stochastic variations in Global Navigation Satellite System (GNSS) height time series is crucial for accurate monitoring of Vertical Land Motions (VLM). This paper studies stochastic variations in daily GNSS height time series in Beijing and its surrounding areas, and explores the contribution of the aperiodic part of environmental (hydrological, non-tidal atmospheric and oceanic) loading deformations to stochastic properties. We utilize the Restricted Maximum Likelihood Estimation (RMLE) method, due to its capability to estimate unbiased stochastic parameters from GNSS time series with offsets. Four metrics are used to evaluate the influence of environmental loading corrections on stochastic properties of 48 GNSS stations, namely: the change in the root mean square (RMS) of residuals, the average power-spectrum characteristics of residuals, temporal and spatial correlation properties of residuals. Results indicate that the average RMS of residuals after loading corrections is reduced by 10.5 %, where non-tidal atmospheric loading constitutes the most pronounced effect with an average RMS reduction ratio of 7.2 %. The notable power reduction within the frequency band ranging from 10 to 50 cycles per year (cpy) is observed after removing loading deformations. Loading corrections result in the increase in white noise amplitudes and the decrease in spectral indices for all stations, and the reduction of modified power-law noise amplitudes for 81 % of GNSS stations, indicating that loading deformations may introduce bias into the parameter estimates of the white noise plus power-law process model. The seasonality of spatial correlation coefficients of residuals is remarkably reduced after loading corrections, verifying that the environmental loading is a significant contributor to common mode errors of GNSS height time series in Beijing and its surrounding areas.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 2","pages":"Pages 734-749"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144471593","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Destabilization mechanisms of electrostatic solitary waves in ion-acoustic regimes within collisionless cometary plasma","authors":"A. Atteya ,&nbsp;Reem Altuijri ,&nbsp;Kottakkaran Sooppy Nisar ,&nbsp;Abdel-Haleem Abdel-Aty ,&nbsp;Eman Mohammed El-Bayoumi","doi":"10.1016/j.asr.2025.05.031","DOIUrl":"10.1016/j.asr.2025.05.031","url":null,"abstract":"<div><div>This study investigates the dynamics of instability and energy of ion-acoustic waves (IAWs) in a magnetized, five-component cometary plasma comprising inertial hydrogen ions (<span><math><mrow><msup><mrow><mi>H</mi></mrow><mrow><mo>+</mo></mrow></msup></mrow></math></span>), positively/negatively nonextensive charged oxygen ions (<span><math><mrow><msup><mrow><mi>O</mi></mrow><mrow><mo>±</mo></mrow></msup></mrow></math></span>), and superthermal-distributed solar/cometary electrons. The work results in deriving the Zakharov-Kuznetsov (ZK) equation under nonextensive ion effects, showing how wave stability and energy transmission are governed by electron superthermality, ion nonextensivity, and magnetic geometry. The findings show that phase velocity increases with solar electron densities and superthermality, but decreases with ion nonextensivity of oxygen ions, emphasizing the competition between the ion-driven dissipation and electron thermal pressure. Increased Landau damping and increased electron pressure cause lower negative oxygen ion density to amplify the instability growth rate, <em>gr</em>, by upsetting charge neutrality and causing ion drifts; higher electron densities, on the other hand, cause <em>gr</em> to increase. Energy, <span><math><mrow><msub><mrow><mi>E</mi></mrow><mrow><mi>n</mi></mrow></msub></mrow></math></span>, accumulates with solar electron density, oblique propagation, <span><math><mrow><mi>θ</mi></mrow></math></span>, and weaker magnetic fields, <span><math><mrow><mi>ω</mi></mrow></math></span>, via enhanced nonlinear steepening and dispersive broadening. In contrast, <em>gr</em> peaks at parallel propagation (<span><math><mrow><mi>θ</mi><mo>→</mo><mn>0</mn><mi>°</mi></mrow></math></span>) but declines at oblique angles (<span><math><mrow><mi>θ</mi><mo>&gt;</mo><msub><mrow><mi>θ</mi></mrow><mrow><mi>c</mi></mrow></msub></mrow></math></span>) as a result of magnetic stabilization. Notably, magnetic fields suppress <em>gr</em> at high <span><math><mrow><mi>θ</mi></mrow></math></span> while enhancing <span><math><mrow><msub><mrow><mi>E</mi></mrow><mrow><mi>n</mi></mrow></msub></mrow></math></span> through wave broadening. The study identifies a critical distinction: <span><math><mrow><msub><mrow><mi>E</mi></mrow><mrow><mi>n</mi></mrow></msub></mrow></math></span> <!-->depends on nonlinearity-dispersion balance, whereas <em>gr</em> hinges on electron–ion coupling and resonant interactions. By connecting microscopic wave activity to macroscopic instability thresholds, these findings provide cometary plasma models forward and help to understand Rosetta mission data and forecast wave-driven heating in cometary environments.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 3","pages":"Pages 1817-1831"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144579347","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Formation of solar spicules due to high-frequency perturbation in the solar photosphere","authors":"Isha Sharma,&nbsp;Disha Varshney,&nbsp;K.A.P. Singh","doi":"10.1016/j.asr.2025.05.028","DOIUrl":"10.1016/j.asr.2025.05.028","url":null,"abstract":"<div><div>Spicules are jet-like structures, visible on the Sun and noticed quite frequently during space-based observations of the solar chromosphere. It is important to understand the physical processes that could lead to the formation of taller spicules having heights larger than 6 Mm. In the present work, we have provided high-frequency photospheric perturbation and studied nonlinear processes in the spicule formation under the framework of magnetohydrodynamics (MHD). Perturbations in the solar photosphere include pressure perturbations and torsional velocity perturbations. The solar spicules in our model are formed due to the interaction of nonlinear MHD waves, specifically slow magneto-acoustic and Alfvén waves with the solar transition region. Through a self-consistent approach and 1.5D MHD simulations, we found that the high-frequency perturbation in the solar photosphere could generate taller spicules if a suitable wave period and height of the solar transition region are considered initially. The simulations are performed over a long time (e.g., up to 800 min), and in certain conditions, we found that the spicule reaches a height of 10 Mm and beyond. Furthermore, high-frequency perturbations play a significant role in forming the spicules and chromospheric heating.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 2","pages":"Pages 1080-1090"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144471678","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Understanding the IBEX ribbon using the kinetic model of pickup proton transport in a scatter-free limit","authors":"Igor I. Baliukin ,&nbsp;Vladislav V. Izmodenov","doi":"10.1016/j.asr.2025.05.030","DOIUrl":"10.1016/j.asr.2025.05.030","url":null,"abstract":"<div><div>One of the most remarkable discoveries by the <em>Interstellar Boundary Explorer (IBEX)</em> is the ribbon – a narrow band of enhanced energetic neutral atom (ENA) fluxes observed in the sky. The prevailing explanation attributes the <em>IBEX</em> ribbon to the secondary ENA mechanism. In this process, “primary” hydrogen ENAs, produced via charge exchange between solar wind protons and interstellar hydrogen atoms within the heliosphere, travel beyond the heliopause and undergo further charge exchange with protons of the local interstellar medium (LISM), generating pickup protons. Some of these pickup protons subsequently experience charge exchange with interstellar hydrogen atoms, forming “secondary” ENAs, some of which travel back toward the Sun and are detected by the <em>IBEX</em>.</div><div>This paper presents a kinetic model developed to simulate secondary ENA fluxes. Ribbon simulations are performed using global distributions of plasma and hydrogen atoms in the heliosphere derived from a kinetic-magnetohydrodynamic model of the solar wind interaction with the LISM. The model accounts for all relevant primary ENA populations, including neutralized thermal solar wind protons, neutralized pickup protons, and ENAs originating in the inner heliosheath. The transport of pickup protons beyond the heliopause is described by the focused transport equation for a gyrotropic velocity distribution in the scatter-free limit, assuming no pitch-angle scattering or energy diffusion.</div><div>Our simulations qualitatively reproduce <em>IBEX-Hi</em> (0.5–6 keV) ribbon observations and exhibit good quantitative agreement at low heliolatitudes. However, the model underestimates fluxes at high heliolatitudes, likely due to the omission of non-stationary solar wind behavior in the stationary framework used in this work. The study highlights the importance of ENAs from the inner heliosheath, a population considered for the ribbon production in the frame of the kinetic model of pickup proton transport in the heliosphere for the first time, for accurately reproducing ribbon fluxes observed by <em>IBEX-Hi</em> at the highest energy steps.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 3","pages":"Pages 1917-1938"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144579441","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Stratigraphic information underneath Chang’e-4 landing area as revealed by the ejecta of Zhinyu crater","authors":"Bingyao Han ,&nbsp;Zongyu Yue ,&nbsp;Sheng Gou ,&nbsp;Huacheng Li","doi":"10.1016/j.asr.2025.05.033","DOIUrl":"10.1016/j.asr.2025.05.033","url":null,"abstract":"<div><div>Zhinyu crater is one of the largest craters in the vicinity of Chang’-4 landing site, and its ejecta features three compositional rings. This indicates that there are at least three layers of mare basalts. The thicknesses of the layers were estimated using empirical equations from previous studies, which are based on the average characteristics of lunar impact craters. Therefore, a specific analysis of the Zhinyu crater is necessary, as it can provide reliable information for establishing regional stratigraphy. We carried out the numerical simulation to the formation process of Zhinyu crater and further analyzed its ejecta distribution. We used the tracers to find the original depth of the ejecta, and we proposed a tracer can be considered as the ejecta if it is subject only to gravitational forces. The strategy was verified with the laboratory experiment. Our result indicates that the thicknesses of the three basalt layers are (from top to bottom) 190 m, 50 m, &gt;60 m, respectively. We also find that some ejecta blocks instead of the continuous ejecta from Zhinyu crater might be encountered by the Chang’e-4 rover (Yutu-2), and the rover will firstly observe the ejecta from shallow subsurface when it traverses towards the crater.</div></div>","PeriodicalId":50850,"journal":{"name":"Advances in Space Research","volume":"76 3","pages":"Pages 1774-1781"},"PeriodicalIF":2.8,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144579353","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}