Planetary and Space Science最新文献

{"title":"A study of very high resolution visible spectra of Titan: Line characterisation in visible CH4 bands and the search for C3","authors":"Rafael Rianço-Silva ,&nbsp;Pedro Machado ,&nbsp;Zita Martins ,&nbsp;Emmanuel Lellouch ,&nbsp;Jean-Christophe Loison ,&nbsp;Michel Dobrijevic ,&nbsp;João A. Dias ,&nbsp;José Ribeiro","doi":"10.1016/j.pss.2023.105836","DOIUrl":"10.1016/j.pss.2023.105836","url":null,"abstract":"<div><p>The atmosphere of Titan is a unique natural laboratory for the study of atmospheric evolution and photochemistry akin to that of the primitive Earth, with a wide array of complex molecules discovered through infrared and sub-mm spectroscopy. Here, we explore high resolution visible spectra of Titan (obtained with VLT-UVES) and retrieve an empirical high resolution list of methane absorption features at high resolution, (<span><math><mrow><mi>R</mi><mo>=</mo><mn>100</mn><mo>.</mo><mn>000</mn></mrow></math></span>) between 5250 Å and 6180 Å, for which no linelists are yet available. Furthermore, we search for the predicted, but previously undetected carbon trimer, C<span><math><msub><mrow></mrow><mrow><mn>3</mn></mrow></msub></math></span>, on the atmosphere of Titan, at its 4051 Å band. Our results are consistent with the presence of C<span><math><msub><mrow></mrow><mrow><mn>3</mn></mrow></msub></math></span> at the upper atmosphere of Titan, with a column density of <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>13</mn></mrow></msup></mrow></math></span> cm⁻². This study of Titan’s atmosphere with high-resolution visible spectroscopy presents a unique opportunity to observe a planetary atmosphere where CH<span><math><msub><mrow></mrow><mrow><mn>4</mn></mrow></msub></math></span> is the main visible molecular absorber, from which CH<span><math><msub><mrow></mrow><mrow><mn>4</mn></mrow></msub></math></span> optical proprieties can be studied. It also showcases the use of a close planetary target to test new methods for chemical retrieval of minor atmospheric compounds, in preparation for upcoming studies of cold terrestrial exoplanet atmospheres.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105836"},"PeriodicalIF":2.4,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0032063323002052/pdfft?md5=11b88a0e45862f58da6c7ba9fb67dbec&pid=1-s2.0-S0032063323002052-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139396980","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":"Chondrules from the ordinary chondrite Itawa Bhopji (L3-5): Noble gases and nitrogen","authors":"Ramakant R. Mahajan","doi":"10.1016/j.pss.2024.105837","DOIUrl":"10.1016/j.pss.2024.105837","url":null,"abstract":"<div><p><span><span>Noble gases and nitrogen compositions are investigated in chondrules<span> of Itawa Bhopji (L3-5) chondrite. Single chondrule and bunch of chondrules were analysed in this work. </span></span>Isotopic ratios of noble gases in chondrules indicate mixture of Q-HL-SW and cosmogenic. The cosmic ray exposure age of the chondrules using </span>²¹<span>Ne are 30.0 ± 2.3 and 25.9 ± 2.5 Ma. No excess cosmic ray exposure (CRE) age observed in the chondrules from that of bulk aliquot of dark lithology. The trapped nitrogen signature, δ</span>¹⁵N_t in the chondrules, is +15.8 ± 2.2‰ (bunch of chondrules) and +15.1 ± 2.3‰ (single chondrule). Trapped nitrogen isotopic signature in chondrules differs from dark and light lithology of the meteorite and it is also distinct from metal separates. Trapped nitrogen composition in chondrules differs than Q-phase, solar wind (SW) and HL components. This implies that chondrules in Itawa Bhopji (L3-5) chondrite composed of isotopically distinct component than any of the known reservoir. Distinct trapped nitrogen isotopic signatures in the constituents of a meteorite indicates their formation at various places with the heliocentric distance. The abundance of nitrogen in chondrules is 6.14 ± 0.51 ppm (bunch) and 5.71 ± 0.48 ppm (single). Radiogenic ¹²⁹Xe from the decay of ¹²⁹I was observed in chondrules, indicative of their formation in early solar system.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105837"},"PeriodicalIF":2.4,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139420653","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":"Lunar spinels in the Aristarchus crater and cobra head","authors":"Yehor Surkov ,&nbsp;Yuriy Shkuratov ,&nbsp;Vadym Kaydash ,&nbsp;Gorden Videen ,&nbsp;Urs Mall ,&nbsp;Sergey Velichko","doi":"10.1016/j.pss.2023.105831","DOIUrl":"10.1016/j.pss.2023.105831","url":null,"abstract":"<div><p>On the lunar surface we identify and map Mg-spinel-bearing deposits on the southern section of the Aristarchus Plateau, including the Aristarchus and Herodotus craters and the Cobra Head using the color rations C (950-750 nm) and C (2650/1550 nm). The main concentrations of spinel-bearing material are located on the peak and floor of the Aristarchus crater, with some minor deposits also detected on the walls. Most of these deposits are associated with surface areas covered by massive boulders. The crater peak reveals a bimodality of spectral characteristics and surface types: The smooth, darker surface of the northernmost face has a strong absorption band near 1 μm that is evidence of mafic mineral presence. The brighter and rougher surface of the peak midportion reveals absorption starting from 1.55 μm. This suggests a dominant plagioclase/Mg-spinel mineralogic composition of Fe-poor minerals. The Mg-spinel deposits outside the crater are represented by a single unit located on the southern slope of the Cobra Head. The intrusive volcanism and further uplifting by the impact is discussed as a possible origin of the Mg-spinel deposits of the region.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105831"},"PeriodicalIF":2.4,"publicationDate":"2023-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0032063323002003/pdfft?md5=ab722bfc84bf2142762c5fe72cb79754&pid=1-s2.0-S0032063323002003-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139028091","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":"Asteroid regolith strength: Role of fine-fractions","authors":"Christopher Cox,&nbsp;Julie Brisset,&nbsp;Aracelis Partida,&nbsp;Alexander Madison,&nbsp;Olivia Bitcon","doi":"10.1016/j.pss.2023.105829","DOIUrl":"https://doi.org/10.1016/j.pss.2023.105829","url":null,"abstract":"<div><p>Most smaller asteroids (<span><math><mo>&lt;</mo></math></span><span><span>1 km diameter) are granular material loosely bound together primarily by self-gravity known as rubble piles. In an effort to better understand the evolution of rubble-pile asteroids, we performed bulk measurements using granular simulant to study the effects of the presence of fine grains on the strength of coarse grains. Our laboratory samples consisted of fine–coarse mixtures of varying percentages of fine grains by volume of the sample. We measured the material’s angle of repose, Young’s Modulus, angle of </span>internal friction<span>, cohesion, and tensile strength by subjecting the samples to compressive and shear stresses. The coarse grains comprising the fine–coarse mixtures ranged from 1 mm to 20 mm (2 cm) and the fines were sieved to sub-millimeter sizes (</span></span><span><math><mo>&lt;</mo></math></span>1 mm). The measured angles of repose varied between 32<span><math><mo>°</mo></math></span>–45<span><math><mo>°</mo></math></span> which increased with increasing fine percentage. In compression, samples generally increased in strength with increasing fine percentage for both confined and unconfined environments. In all cases, the peak strengths were not for purely fine grains but for a mixture of fine and coarse grains. Shear stress measurements yielded angles of internal friction ranging between 25<span><math><mo>°</mo></math></span> and 45<span><math><mo>°</mo></math></span><span> with a trend opposite that of the angle of repose, 300–550 Pa for bulk cohesion, and 0.5–1.1 kPa for tensile strength. Using other published works that include data from telescopic and in-situ observations as well as numerical simulations, we discussed the implications of our findings regarding rubble-pile formation, composition, evolution, and disruption. We find that the presence of fine grains in subsurface layers of regolith on an asteroid (confined environment) aids the avoidance of disruption due to impact. However these same fines increase an asteroid’s chance to disrupt or deform from high rotation speeds due to reduced grain interlocking. In surface layers (unconfined environments), we find that the presence of fine grains between coarse ones generates stronger cohesion and aids in the prevention of mass loss and surface shedding.</span></p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105829"},"PeriodicalIF":2.4,"publicationDate":"2023-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138633464","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":"Planar spacecraft trajectories in the Didymos–Dimorphos binary asteroid system","authors":"G. Voyatzis,&nbsp;D. Karydis,&nbsp;I. Gkolias,&nbsp;M. Gaitanas,&nbsp;K. Tsiganis","doi":"10.1016/j.pss.2023.105825","DOIUrl":"10.1016/j.pss.2023.105825","url":null,"abstract":"<div><p><span><span>The dynamics of a spacecraft in the vicinity of the Didymos and Dimorphos binary system is studied, with specific emphasis on the bounded orbits that exist in such a perturbed gravitational environment. The binary environment is approximated with gradually increasing fidelity, starting with a model that simulates Didymos with an oblate spheroid and Dimorphos with a triaxial ellipsoid. Within these simplifying assumptions, we compute all the families of planar periodic orbits and we study the deviations that arise to them under more realistic perturbations that include the actual shape of Didymos, its rotation, the solar gravity and radiation pressure. To establish the robustness of the different orbital configurations, we perform a classification based on planar dynamical maps and connect the stability regions with the periodic motion. A subset of </span>retrograde orbits around Didymos and a particular type of outer orbits with double multiplicity seem to show long-term stability and robustness, so they can be assumed as safe orbits. On the contrary, orbits around Dimorphos, although stable in the basic model, become strongly unstable in our more realistic model. Our approach is based only on natural dynamics and no active </span>spacecraft control is applied, thus providing a useful methodology in finding ‘safe’ orbits for a spacecraft in the vicinity of a binary asteroid system.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105825"},"PeriodicalIF":2.4,"publicationDate":"2023-12-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138581799","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":"Age estimation and boulder population analysis of the West crater at Apollo 11 landing site using Orbiter High Resolution Camera on board Chandrayaan-2 mission","authors":"Rohit Nagori,&nbsp;Aditya K. Dagar,&nbsp;R.P. Rajasekhar","doi":"10.1016/j.pss.2023.105828","DOIUrl":"https://doi.org/10.1016/j.pss.2023.105828","url":null,"abstract":"<div><p><span>Orbiter High Resolution Camera (OHRC) on-board Chandrayaan-2 had acquired a high-resolution image (∼0.26 m) covering Apollo 11 landing site, showing the Lander<span><span> Module (LM) along with other small-scale features, such as boulders, etc. In the east of Apollo 11 LM lies the West crater, which has a rich population of boulders spread around it. We studied this boulder distribution around the West crater to estimate the age of the West crater and to understand the aspects related to the impact cratering and space weathering through the analysis of boulder distribution. For this, we identified and mapped &gt;8500 boulders around the West crater using the OHRC image, out of which 6466 boulders (&gt;∼1 m in size) lying within 1–5 crater radius were used for further analysis. For estimating the age of the West crater, we applied various methods based on crater morphology, boulder distributions and Diviner Rock Abundance. The age was estimated to be in the range of 80 Ma to 120 Ma with the most probable age close to 100 Ma, the same as that expected from the cosmic ray exposure dating. Boulder distribution around the West crater was found to be highly anisotropic with majority of boulders lying in the eastern to north-eastern direction, suggesting an impact at very low angle. Relationship between crater size and largest boulder size also pointed towards primary origin of the West crater. The Height (H) to Diameter (D) ratio is estimated to be ∼0.25 considering all the boulders with diameter ≤ 4m, going up to 0.38 with comparatively poor correlation for boulders with diameter &gt; 4m. The H/D ratio from Apollo mission photos for boulders around Apollo 11 LM is found to be approximately double that of the corresponding measurements from the OHRC image. We also fit a Power law and the Weibull distribution to the cumulative Boulder Size </span>Frequency Distribution (BSFD) curve with Maximum Likelihood (ML) method and Kolmogrov-Smirnoff (KS) statistics. Both fit well with R</span></span>² of 0.999, but varying minimum diameter (d_KS) of 1.85 m and 1.64 m, respectively. The good fit by Power-law with high slope value (<span><math><mrow><mi>b</mi></mrow></math></span> = 4.61) describes the fragmentation due to the West crater forming impact as complex. However, the higher diameter tail was better explained by the Weibull fit implying sequential fragmentation of boulders with time.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105828"},"PeriodicalIF":2.4,"publicationDate":"2023-12-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138577512","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":"Orbital evolution and possible parent asteroids of 40 instrumentally observed meteorites","authors":"Filip Hlobik,&nbsp;Juraj Tóth","doi":"10.1016/j.pss.2023.105827","DOIUrl":"10.1016/j.pss.2023.105827","url":null,"abstract":"<div><p><span>We present the orbital evolution of 40 meteorites with known heliocentric orbits, both nominal and their clones as well. The goal of our work was to determine the stability of their orbits and to find possible connections with known near-Earth asteroids. Stability along with a probability of a random association were used to select probable candidates. We have found stable behaviour of orbits for 21 meteorites in the time interval of 100,000 years to the past (e.g. Neuschwanstein, Jesenice). Twelve meteorites displayed different orbital evolution of the nominal orbit and the clones (e.g. Almahata Sitta, Motopi Pan), but in general they were stable. There were seven meteorites on unstable orbits; 3 meteorites exhibited chaotic clone evolutions (Košice, Maribo and Novato) and 4 were on overall unstable orbits (Příbram, Sutter’s Mill, Flensburg and Arpu Kuilpu). This study suggests possible parent bodies from the currently known NEA population for 27 meteorites with very low </span><span><math><msub><mrow><mi>D</mi></mrow><mrow><mi>S</mi><mi>H</mi></mrow></msub></math></span> values and low probabilities of random association.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105827"},"PeriodicalIF":2.4,"publicationDate":"2023-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138553231","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":"The Luna structure, India: A probable impact crater formed by an iron bolide","authors":"K.S. Sajinkumar ,&nbsp;S. James ,&nbsp;G.K. Indu ,&nbsp;Saranya R. Chandran ,&nbsp;Devika Padmakumar ,&nbsp;J. Aswathi ,&nbsp;S. Keerthy ,&nbsp;M.N. Praveen ,&nbsp;N. Sorcar ,&nbsp;J.K. Tomson ,&nbsp;Anil Chavan ,&nbsp;Subhash Bhandari ,&nbsp;M. Satyanarayanan ,&nbsp;R. Bhushan ,&nbsp;A. Dabhi ,&nbsp;Y. Anilkumar","doi":"10.1016/j.pss.2023.105826","DOIUrl":"10.1016/j.pss.2023.105826","url":null,"abstract":"<div><p><span><span>The Luna<span> structure of India has been rumored to be an impact crater for more than a decade without any convincing evidence. This structure (1.5–1.8 km) is prominently visible in the low-lying Banni Plains of the tectonically active Kutch Basin as a circular morphological feature with a less-prominent rim. Luna area is strewn with melt-like rocks having high specific gravity and displaying wide range of </span></span>magnetic properties. It contains minerals like wüstite, kirschsteinite, ulvöspinel, </span>hercynite<span><span>, and fayalite. The </span>whole rock analysis<span> denotes PGE enrichment, with notably higher average concentrations of Ru (19.02 ppb), Rh (5.68 ppb), Pd (8.64 ppb), Os (6.03 ppb), Ir (10.63 ppb) and Pt (18.31 ppb). The target is not exposed at Luna, owing to the overlying thick sequence of Quaternary sediments. The mineralogical and geochemical signatures points to an impact into a target, which is rich in clay with elevated calcium and silica (sand/silt) content. Geochemical data suggests an iron or stony-iron meteorite as the potential projectile at Luna. The silt layer containing plant remnants, underlying the strewn layer, yielded a radiocarbon age of 6905 years, making Luna the biggest crater to result from an iron bolide within the last 10,000 years.</span></span></p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"240 ","pages":"Article 105826"},"PeriodicalIF":2.4,"publicationDate":"2023-12-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138532250","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":"Lunar spinels in the Aristarchus crater and cobra head","authors":"Y. Surkov, Yuriy G. Shkuratov, V. Kaydash, G. Videen, Urs Mall, Sergey Velichko","doi":"10.1016/j.pss.2023.105831","DOIUrl":"https://doi.org/10.1016/j.pss.2023.105831","url":null,"abstract":"","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"217 ","pages":""},"PeriodicalIF":2.4,"publicationDate":"2023-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139013872","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":"Differential aperture photometry and digital coronagraphy with PRAIA","authors":"M. Assafin","doi":"10.1016/j.pss.2023.105816","DOIUrl":"https://doi.org/10.1016/j.pss.2023.105816","url":null,"abstract":"<div><p><span>PRAIA</span><span> – Package for the Reduction of Astronomical Images Automatically – is a suite of photometric and astrometric tasks designed to cope with huge amounts of heterogeneous observations with fast processing, no human intervention, minimum parametrization and yet maximum possible accuracy and precision. It is the main tool used to analyse astronomical observations by an international collaboration involving Brazilian, French and Spanish researchers under the Lucky Star umbrella for Solar System studies. Here, we focus on the concepts of differential aperture photometry and digital coronagraphy underneath </span><span>PRAIA</span><span><span>, used in the reduction of stellar occultations, rotational light curves, mutual phenomena and </span>natural satellite observations. We highlight novelties developed by us and never before reported in the literature, which significantly enhance the precision and automation of photometry and digital coronagraphy, such as: (a) </span><span>PRAIA</span>’s pixelized aperture photometry (<span>PCAP</span>), which avoids pixel sub-sampling or fractioning; (b) fully automatic object detection and aperture determination (<span>BOIA</span><span>), which abolishes the use of arbitrary sky background sigma factors, and finds better apertures than by using subjective FWHM factors; (c) better astrometry improving the aperture and coronagraphy centres, including the new Photogravity Center Method besides circular and elliptical Gaussian and Lorentzian generalized profiles; (d) coronagraphy of faint objects close to bright ones and vice-versa; e) use of elliptical rings for the coronagraphy of elongated profiles; (f) refined quartile ring statistics; (g) multiprocessing image capabilities for faster computation speed. We give examples showing the photometry performance, discuss the advantages of </span><span>PRAIA</span> over other popular packages for Solar System differential photometric observations, point out the uniqueness of its digital coronagraphy in comparison with other coronagraphy tools and methods, and comment about future planed implementations. Besides Solar System works, <span>PRAIA</span><span><span> can also be used in the differential photometry of variable and cataclysmic stars and transient phenomena like exoplanet transits and </span>microlensing, and in the digital coronagraphy of astrophysical observations. </span><span>PRAIA</span> codes and input files are publicly available for the first time at: <span>https://ov.ufrj.br/en/PRAIA/</span><svg><path></path></svg>.</p></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"239 ","pages":"Article 105816"},"PeriodicalIF":2.4,"publicationDate":"2023-11-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138430966","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}