Planetary and Space Science最新文献

{"title":"Geological history of Theia Mons, Beta Regio plume, Venus: Recognition of two main magmatic centers for flows, radiating dyke swarms and triple junction rifting","authors":"A.S. Shimolina ,&nbsp;R.E. Ernst ,&nbsp;H. El Bilali ,&nbsp;D.G. Malyshev ,&nbsp;V.E. Rozhin ,&nbsp;E.G. Antropova","doi":"10.1016/j.pss.2025.106050","DOIUrl":"10.1016/j.pss.2025.106050","url":null,"abstract":"<div><div>Theia Mons (centered at 23.4° N, 79.4° W) is the main volcanic center for the Beta Regio plume, of the Beta-Atla-Themis (BAT) region, Venus. Synthetic aperture radar data (SAR) and altimetry data from the 1989–1994 NASA Magellan mission were used to produce a geological map and history of Theia Mons, revealing two distinct magmatic centers (200 km apart), each the focus of basaltic lava flows, extensional lineaments (representing the surface expression of dyke swarms), and associated rift zones. The study area spans 88°W to 72°W, 16°45′N to 29°45′N, and mapping was at 1:500,000 scale. Our detailed mapping makes this area a prime target for the future Venus missions (orbital and lander), also given that Beta Regio is a strong candidate for ongoing volcanic activity.</div><div>Lava (basaltic) flow units (88 distinguished on the basis of variation in radar backscatter) belonging to Theia Mons volcano were combined into 19 Flow Groups and then into 3 Flow Packages. The lava flows appear to diverge from two distinct magmatic centers, labelled Center 1 (24.5°N, 78.1°W) and Center 2 (23.4° N, 79.4°W), with the older Center 1 being obscured by the volcanism of the younger Center 2. Center 1 consists of flows with low radar brightness and which extend to a maximum to 830 km from the center. Center 2 coincides with the currently preserved central caldera and consists of lava flows of low radar brightness with a maximum length of 620 km, followed by a second pulse of radar-bright flows that are less extensive and concentrated near the center.</div><div>About 10,000 extensional lineaments (grabens, fissures, and fractures) were mapped and grouped into 19 systems, of which 15 are interpreted to overlie dyke swarms: 2 radiating systems are associated with Centers 1 and 2, and 13 other systems belong to other (older and likely unrelated) magmatic centers in the region. A partial circumferential swarm may also be present, associated with Center 2.</div><div>Four other extensional lineaments sets are inferred to represent sets of normal faults associated with rift zones (Devana and Zverine, and additional rift zones). These rift zones exhibit two sets of ‘triple junction’ geometry, which are approximately also focussed on the same Centers 1 and 2, revealed by the lava flows and rift zones.</div><div>An underlying mantle plume is interpreted to be responsible for the dykes, flows and triple junction rifting. The cause of the shift between Centers 1 and 2 (200 km to SW) is unknown, but plausible mechanisms include a shift of the lithospheric plate above a stationary single plume, or a bending of the mantle plume (e.g. in a mantle wind) between timing of Center 1 and Center 2 activity.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106050"},"PeriodicalIF":1.8,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284621","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":"Low temperature fluorescence excitation and emission spectra of molecules relevant to Mars: Chlorobenzene, benzoic acid, phthalic acid, mellitic acid, and benzene in water ice solutions at temperatures between 78 K and 273 K","authors":"Suresh Sunuwar,&nbsp;Carlos E. Manzanares","doi":"10.1016/j.pss.2025.106054","DOIUrl":"10.1016/j.pss.2025.106054","url":null,"abstract":"<div><div>The discovery of chlorobenzene detected in soil samples obtained in Mars has been the subject of several interpretations. The original sample was subjected to pyrolysis before the gas chromatography-mass spectrometry (GC-MS) separation and identification with the Sample Analysis at Mars (SAM) instrument on the Curiosity rover. It is believed that chlorobenzene detected at concentrations above the background level of the instrument was a product of other organic molecules reacting with perchlorates of the Martian soil. Mars surface temperatures may reach a high of about 293 K at noon, at the equator, and a low of about 120 K at the poles. In this paper, characteristic fluorescence excitation and emission spectra are presented for chlorobenzene and the suggested precursor molecules: benzoic acid, phthalic acid, and mellitic acid in transparent hexagonal water ice solutions at temperatures between 273 K and 78 K. In addition, the liquid solution spectra at 292 K. Spectra of benzene in water ice solutions have also been included. The experimental results presented in this paper are to be compared with fluorescence experiments of Mars missions that will explore the polar regions and other regions where water ice is expected to be found. Limits of detection at part per billion by mass (ng/g) concentrations at room temperature are discussed based on our results and the literature. The application of fluorescence for low temperature studies of Mars samples is also discussed with a proposed miniature instrument with a laser source to increase the sensitivity of the detection and could be used for solid or liquid samples.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106054"},"PeriodicalIF":1.8,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284560","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 Arctic analogue for the future exploration of possible biosignatures on Enceladus","authors":"F. Franchi ,&nbsp;M. Túri ,&nbsp;G. Lakatos ,&nbsp;K.K. Rahul ,&nbsp;D.V. Mifsud ,&nbsp;G. Panieri ,&nbsp;R. Rácz ,&nbsp;S.T.S. Kovács ,&nbsp;E. Furu ,&nbsp;R. Huszánk ,&nbsp;R.W. McCullough ,&nbsp;Z. Juhász","doi":"10.1016/j.pss.2025.106051","DOIUrl":"10.1016/j.pss.2025.106051","url":null,"abstract":"<div><div>Methane-rich emissions to the seafloor along the Arctic mid-oceanic ridge hold strong astrobiological significance, as they may represent analogues of putative hydrothermal vent environments on Enceladus. Although such environments on Enceladus would be ideal to sample in future astrobiological missions, this may not be possible due to technological and logistical limitations. As such, searching for biosignatures in the more readily sampled cryovolcanic plumes or Enceladus’ icy shell is preferable. In this regard, the Arctic Ocean, where the geologically active seafloor is covered by thousands of metres of salty water and sealed by an ice cap, is a unique terrestrial analogue of Enceladus. In the present study, we have sought to determine whether any geochemical biosignatures associated with methane cycling (e.g., elevated methane concentrations, carbon isotopic fractionation) can be detected in Arctic ice and seawater samples using mass spectrometric techniques similar to those likely to be included in the payloads of planned missions to Enceladus. Our results have shown that, although no unequivocal evidence of methane could be detected in our Arctic samples, the carbon isotopic composition of carbon dioxide gas and the oxygen isotopic composition of water vapour emitted from the Arctic samples could indeed be measured. Furthermore, an excess of molecular hydrogen with abundances comparable to the composition of Enceladus’ southern pole plume was possibly observed in one of the Arctic ice samples. These results have implications for detectable indirect geochemical evidence of putative ecosystems of hydrogenotrophic methanogenic life on the seafloor of Enceladus and justify future efforts at method development and refinement using apparatus similar to that likely to be included in the payloads of future missions.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106051"},"PeriodicalIF":1.8,"publicationDate":"2025-01-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284622","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":"Closed depressions on the surface of the Moon","authors":"Eulogio Pardo-Igúzquiza ,&nbsp;Peter Dowd","doi":"10.1016/j.pss.2025.106049","DOIUrl":"10.1016/j.pss.2025.106049","url":null,"abstract":"<div><div>This paper provides a new view of the lunar surface by using maps of its closed depressions which are not limited to impact craters. On the lunar landscape, in addition to impact craters of all sizes, there is a rich variety of other types of closed depressions related to impact, volcanism, tectonics and gravitational processes. Kilometre-scale closed depressions have been identified, delineated and mapped on the surface of the Moon by using the digital elevation model provided by the Lunar Orbiter Laser Altimeter (LOLA) instrument onboard the Lunar Reconnaissance Orbiter (LRO) spacecraft together with a pit filling algorithm. The map of closed depressions is a raster map of the same size and spatial resolution as the digital elevation model used to generate it and each pixel provides the depth with respect to the rim of the depression. A number of test sites were chosen to illustrate the methodology including impact basins, maria, highlands, volcanic terrain, intermediate terrain and modified terrain. These maps of closed depressions can be analysed in terms of their location, abundance, size, orientation, depth, geometry, asymmetry and irregularity together with other morphometric parameters. On average, 71% of the surface of the Moon is covered by closed depressions and that number decreases to around 55% for volcanic terrains. The histogram of the depths of the highlands test site can be considered as the standard depth histogram in which impact craters of all sizes cover the entire terrain. The histograms of the other zones vary from that standard profile. The ultimate purpose of this paper is to provide a tool for mapping closed-depressions on the lunar surface which may assist planetary geologists to identify geological processes and recognize geological formations in the study of the geology and geomorphology of the Moon.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106049"},"PeriodicalIF":1.8,"publicationDate":"2025-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284559","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 dynamics of Atlas (S XV): Its current orbit and the recent past","authors":"Demétrio Tadeu Ceccatto ,&nbsp;Nelson Callegari Jr. ,&nbsp;Gabriel Teixeira Guimarães ,&nbsp;Karyna Gimenez","doi":"10.1016/j.pss.2024.106016","DOIUrl":"10.1016/j.pss.2024.106016","url":null,"abstract":"<div><div>This study comprehensively analyzes Atlas’s current orbit, focusing on the secular and resonant perturbations caused by Prometheus, Pandora, and Saturn’s oblateness. We performed numerical integration of the exact equations of motion for a dense ensemble of Atlas clone satellites. Through spectral analysis and interpretation of these orbits on dynamical maps, we identified the domain of the 54:53 Prometheus–Atlas and 70:67 Pandora–Atlas mean-motion resonances, showing that Atlas lies on the boundary of the separatrices of each of these resonances. We also identified the domains for the multiplets <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span> and <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>4</mn></mrow></msub></math></span> associated with 70:67 resonance. Additionally, we explored the variation in Prometheus’s eccentricity, demonstrating that as eccentricity increases (or decreases) in the 54:53 resonance domain correspondingly decreases (or increases). This combined analysis, between the above mappings, revealed qualitatively the overlap between the 54:53 and 70:67 resonances, which are responsible for the chaotic behavior of Atlas’s orbit. We quantified chaotic motion in frequency space and found that the vicinity of Atlas is characterized by weak to moderate chaos, rather than strong chaos. Finally, we investigated Atlas’s recent past, considering Prometheus’s migration under the influence of Saturn’s tidal forces. This analysis reveals several resonances crossed in the past, particularly focusing on the Atlas–Prometheus pair, which exhibited a co-orbital configuration.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106016"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176544","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":"Two methods for determining the temperature on the surface of the cometary nucleus based on spectroscopic measurements","authors":"Marcin Wesołowski ,&nbsp;Piotr Potera ,&nbsp;Krzysztof Kucab","doi":"10.1016/j.pss.2024.106027","DOIUrl":"10.1016/j.pss.2024.106027","url":null,"abstract":"<div><div>The paper presents two methods that can be used to determine the surface temperature of a cometary nucleus. The key role in this approach is played by the measurement of hemispherical albedo for selected dust analogues, which was performed using a Cary 5000 spectrometer. To most accurately reflect the actual structure of the dust layer present on the surface of the cometary nucleus under Earth’s conditions, selected dust analogues were used in laboratory research. In the first method, bolometric albedo (Bond albedo) was used, and in the second method, hemispherical albedo was used, which comes directly from the measurement. Comparing both methods, it was found that the average value of the temperature difference for a given analogue is 0.47 K. Due to the small temperature differences between these approaches, both methods can be treated as equivalent. Based on the measurements and calculations performed, it was found that the most representative analogue of the actual dust present on the surface of comet 67P/Churyumov–Gerasimenko is a sample consisting of a mixture of sand with a volume fraction of about 10% and charcoal with a volume fraction of about 90%.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106027"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176546","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":"Cycles of change: Long and short term aeolian evolution at the Olympus Maculae, Mars","authors":"Kirby Runyon ,&nbsp;Charlie Detelich ,&nbsp;Kim Seelos ,&nbsp;Christina Viviano ,&nbsp;Debra Buczkowski ,&nbsp;Ryan O’Connor ,&nbsp;Jessica Harryman ,&nbsp;Adriana Peña","doi":"10.1016/j.pss.2024.106013","DOIUrl":"10.1016/j.pss.2024.106013","url":null,"abstract":"<div><div>The low-dust Olympus Maculae are a unique geologic window to the local volcanic and aeolian stratigraphy on Mars. The Maculae display dust-cover changes associated with the 2018 global dust storm and dust devils confined to the dark maculae. Regional yardangs and sand patches indicate erosion and deposition and thus strong wind, yet we have not observed meter-scale ripple movement within the dark sand deposits nor decameter-scale ripple movement more regionally. On longer timescales, yardangs along a continuum of morphologies point to cycles of abrasion, infilling, lithification, and re-abrasion. Together, the dust changes and yardang evolution bracket the timescales for landscape evolution in and around the Maculae.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106013"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177378","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":"Precision in planetary exploration: Crater detection with residual U-Net34/50 and matching template algorithm","authors":"Ritik Raju Mohite ,&nbsp;Sushil Kumar Janardan ,&nbsp;Rekh Ram Janghel ,&nbsp;Himanshu Govil","doi":"10.1016/j.pss.2024.106029","DOIUrl":"10.1016/j.pss.2024.106029","url":null,"abstract":"<div><div>Counting craters on celestial bodies such as the Moon is essential for understanding the Solar System's evolution and its dynamic past. The conventional crater recognition methods rely heavily on human observation, often paired with standard machine learning techniques. However, these methods face obstacles, like the absence of an objective criterion and challenges in achieving accurate recognition results for overlapping or smaller craters. To mitigate these issues, our proposed solution involves implementing a convolutional neural network known as the Residual U-Net-34 and Residual U-Net-50. These models are designed to effectively identify craters within lunar Digital Elevation Model (DEM) images. The initial step of our method involves the emphasizing of crater edges and suppressing the other surfaces within lunar DEM data. Following edge detection, we employ matching template algorithm to calculate the size and positions of craters within the lunar DEM data. In the Residual U-Net-34 and Residual U-Net-50 architectures, the framework extends the U-Net model by incorporating the residual convolution block, departing from conventional convolution methods. This hybridization leverages the strengths of both U-Net and residual networks. Remarkably, Residual U-Net-34 and Residual U-Net-50 maintains the input and output image sizes, simplifying the training process due to its use of residual units. This design also enables straightforward optimization of the proposed model. The approach focuses on crater rims and demonstrates the ability to identify overlapping craters. Within the domain of lunar crater recognition, our model demonstrates elevated performance with a recall of 77.22% and precision of 83.67% when operating on DEM data. Notably, the recall and precision outperform other deep learning methods. These experimental outcomes validate the feasibility of leveraging our network for crater recognition within lunar DEM datasets.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106029"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176542","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":"Engineering models of turbulence in the Venus atmosphere: Application to DAVINCI and other missions","authors":"Ralph Lorenz","doi":"10.1016/j.pss.2024.106030","DOIUrl":"10.1016/j.pss.2024.106030","url":null,"abstract":"<div><div>A model of turbulence in the Venus atmosphere is developed for simulating the dynamics of vehicles such as balloons or descent probes, with particular application to the low-latitude daytime descent of the DAVINCI probe currently in development. A discrete ‘random-walk’ turbulence formulation of continuous gusts is used, which offers simple implementation for numerical flight simulations. The model is validated against Doppler observations of the Venera 11 and 12 landers and other data, and some features and challenges of interpreting models and observations are discussed. Model parameter variations as a function of latitude and local time are suggested.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106030"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176545","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":"Geomorphological study of the gullies in Penticton Crater, Mars: Classification and origin","authors":"Varsha Natarajan,&nbsp;Kusuma K N,&nbsp;D Lekshmi Nandana","doi":"10.1016/j.pss.2024.106014","DOIUrl":"10.1016/j.pss.2024.106014","url":null,"abstract":"<div><div>Penticton crater, a southern hemisphere mid-latitude crater on Mars, is covered with features that are typical examples of Martian gullies that resemble the terrestrial gullies on Earth. We studied the gullies present in the Penticton crater, classified them and interpreted their formation mechanism using a remote sensing approach. A wide variety of gullies, including the classic gullies, channel gullies, alcove-apron features, linear gullies and a distinct light-toned gully, were detected in the crater. With its diverse classes of gullies and absence of a preferential orientation trend between pole-facing and equator-facing slopes, the Penticton crater is ideal for observing present-day gully activity and studying the mechanism of modern gully formation. The geomorphological study points out prominent glacial features like lobate debris apron (LDA), lineated valley fill (LVF), and concentric crater fill (CCF) in the region. Extensive morphologic evidence suggests the previous existence of latitude-dependent mantle (LDM) on the pole-facing crater walls. The morphometric analysis using parameters like length, orientation, alcove and apron width of the gullies for all four Martian seasons suggests that the gullies are currently not active. The age estimated using crater size frequency distribution indicated that the study area is 5.5 ± 0.7 Ma, which falls in the range of the high obliquity period of Mars. We propose a rare scenario where there are multiple gully-forming mechanisms acting on the same crater. Our results imply that the gullies on the pole-facing slopes are formed on LDM due to destabilization triggered by the sublimation during the recent shift in Martian obliquity. However, morphometric parameters, including the apex slopes suggest that the gullies on the steeper equator-facing slope were most likely formed by the sliding of dry granular sand.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106014"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177377","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}