Planetary and Space Science最新文献

{"title":"Geological mapping and characterization of the NW-Phoebe volcano-magmatic center on Venus","authors":"E.G. Antropova ,&nbsp;C.H.G. Braga ,&nbsp;R.E. Ernst ,&nbsp;H. El Bilali ,&nbsp;J.W. Head ,&nbsp;K.L. Buchan ,&nbsp;A. Shimolina","doi":"10.1016/j.pss.2024.105996","DOIUrl":"10.1016/j.pss.2024.105996","url":null,"abstract":"<div><div>Detailed geological mapping (at 1:500,000 scale) of the area located in the eastern part of the BAT region, northwest of Phoebe Regio (∼4°N to 1°S; ∼85° to 78°W) using Magellan SAR images has distinguished 48 volcano-tectonic units and 22 structural units. Stratigraphically, the oldest units are represented by fragments of the tesserae, densely lineated plains and other plains units. Younger units include lobate flow fields oriented in various directions (NE, E, SW) and flows associated with shield clusters.</div><div>The post-tesserae evolutionary model proposed for this region distinguishes two Stages, early (I) and late (II), and explains the sequence of formation of all the geological features in terms of intraplate magmatism. Stage I consists of multiple corona structures and associated volcanism that are widely dispersed over the study area. Stage II consists of an intermediate-scale volcano with multiple lava flows radiating approximately from its center, and a field of small shield volcanoes near the summit. The units of Stage II appear to be approximately coeval and to define a distinct volcanic event covering an areal extent of ⁓250,000 km², that we have termed the NW-Phoebe event.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105996"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142746080","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":"Modeling the interstellar dust detections by DESTINY+ I: Instrumental constraints and detectability of organic compounds","authors":"Harald Krüger ,&nbsp;Peter Strub ,&nbsp;Maximilian Sommer ,&nbsp;Georg Moragas-Klostermeyer ,&nbsp;Veerle J. Sterken ,&nbsp;Nozair Khawaja ,&nbsp;Mario Trieloff ,&nbsp;Hiroshi Kimura ,&nbsp;Takayuki Hirai ,&nbsp;Masanori Kobayashi ,&nbsp;Tomoko Arai ,&nbsp;Jon Hillier ,&nbsp;Jonas Simolka ,&nbsp;Ralf Srama","doi":"10.1016/j.pss.2024.106010","DOIUrl":"10.1016/j.pss.2024.106010","url":null,"abstract":"<div><div>The DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> spacecraft will be launched to the active asteroid (3200) Phaethon in 2025. The spacecraft will be equipped with the DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> Dust Analyzer (DDA) which will be a time-of-flight impact ionization mass spectrometer. In addition to the composition of impacting dust particles, the instrument will measure the particle mass, velocity vector, and surface charge. Here, we study the detection conditions of DDA for interstellar dust during the DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> mission. We use the interstellar dust module of the Interplanetary Meteoroid environment for EXploration model (IMEX Sterken et al., 2013; Strub et al., 2019) to simulate the flow of interstellar dust through the Solar System. Extending earlier work by Krüger et al. (2019b) we consider the entire DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> mission, i.e. the Earth-orbiting phase of the spacecraft during the initial approximately 1.5 years after launch, the nominal interplanetary mission phase up to the Phaethon flyby, and a four-years mission extension beyond the Phaethon flyby. The latter may include additional asteroid flybys. For predicting dust fluxes and fluences we take into account a technical constraint for DDA not to point closer than <span><math><mrow><mn>90</mn><mo>°</mo></mrow></math></span> towards the Sun direction for health and safety reasons of the instrument and in order to avoid electrical noise generated by photoelectrons. For the Earth orbiting phase after launch of DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> our simulations predict that up to 28 interstellar particles will be detectable with DDA in 2026. In the following years the interplanetary magnetic field changes to a focussing configuration for small (<span><math><mrow><mo>≲</mo><mn>0</mn><mo>.</mo><mn>1</mn><mspace></mspace><mi>μ</mi><mi>m</mi></mrow></math></span>) interstellar dust particles. This increases the total number of detectable particles to 50 during the interplanetary mission of DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> in 2027. In 2028 and 2029/30 approximately 160 and 190 particles will be detectable, respectively, followed by about 500 in 2030/31. We also make predictions for the detectability of organic compounds contained in the interstellar particles which is a strong function of the particle impact speed onto the detector. While organic compounds will be measurable only in a negligible number of particles during the Earth orbiting and the nominal interplanetary mission phases, a few 10s of interstellar particle detections with measurable organic compounds are predicted for the extended mission from 2028 to 2031.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 106010"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142746082","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":"Induced polarization in the transient electromagnetic method for detection of subsurface ice on Earth, Mars, and the Moon","authors":"Erlend Finden ,&nbsp;Roar Skartlien ,&nbsp;Sverre Holm ,&nbsp;Svein-Erik Hamran","doi":"10.1016/j.pss.2024.106007","DOIUrl":"10.1016/j.pss.2024.106007","url":null,"abstract":"<div><div>The transient electromagnetic method (TEM) can capture an induced polarization (IP) signature of subsurface ice. Using numerical modeling of a horizontally layered earth, we investigate how IP in TEM can be exploited for subsurface ice detection on Earth, Mars, and the Moon. In the model we implement electrical parameters from laboratory measurements of ice, planetary regolith simulants, and terrestrial soil from the literature. In contrast to currently applied forward models, we include two Cole–Cole relaxation terms to model the dielectric relaxation of adsorbed water or salt hydrate in addition to the relaxation of ice. On Earth, IP signals of shallow layers of silt mixed with 44–100 vol% ice embedded in resistive host layers of 3 k<span><math><mi>Ω</mi></math></span>m can be detected. Both at mid (45<span><math><msup><mrow></mrow><mrow><mo>∘</mo></mrow></msup></math></span> N) and lower (35<span><math><msup><mrow></mrow><mrow><mo>∘</mo></mrow></msup></math></span> N) latitudes on Mars, meter thick layers of massive ice can be detected at 10 m depth if the ice contains salts. Corresponding layers of 60 vol% ice mixed with Martian regolith simulant show similar detectability. For IP signals of lunar ice to be detected in ice volume fractions of 7.4%–46%, a development in TEM technology is required, including mitigation of early time interference, or enhancing the signal to noise level.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 106007"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142746081","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":"Asymmetrical distribution of 1–20 km craters on the Moon","authors":"Chenxu Zhao ,&nbsp;Zongyu Yue ,&nbsp;Kaichang Di ,&nbsp;Yutong Jia ,&nbsp;Wing-Huen Ip ,&nbsp;Yangting Lin ,&nbsp;Bo Wu ,&nbsp;Biao Wang ,&nbsp;Bin Xie","doi":"10.1016/j.pss.2024.106015","DOIUrl":"10.1016/j.pss.2024.106015","url":null,"abstract":"<div><div>Previous studies have provided evidence for the synchronous rotation induced cratering asymmetry on lunar surface through numerical simulations and statistical analysis of a limited number of fresh craters. In this study, we reevaluated cratering asymmetry in lunar highland from (70°W, 60°N) to (70°E, 60°S) region using a new crater catalogue with diameters (D) ranging from 1 to 20 km. By utilizing a depth-to-diameter (d/D) ratio constraint to exclude the interference of degraded and secondary craters, we observed significant asymmetry in craters with d/D &gt; 0.15. Moreover, leveraging the characteristic that larger diameter craters (D &gt; 7 km) are less susceptible to degradation, we observed a more pronounced asymmetry with increasing diameter. Particularly, impact craters with larger D and d/D ratios (D &gt; 7 km, d/D &gt; 0.15) displayed an asymmetrical longitudinal distribution, aligning with predictions from the theoretical model. In the diameter range of 10 km–20km, for craters with d/D &gt; 0.15, we observed that new crater influx occurring after 4.0 Ga years ago contributed little to this particular crater population. Therefore, we suggest that the cratering asymmetry was already present before 4.0 Ga. Due to the non-uniform ejecta from the Orientale Basin onto the highland regions, a significant number of smaller impact craters (1–5 km) have degraded or disappeared in the leading region, thereby diminishing the manifestation of the cratering asymmetry. The pronounced asymmetry exhibited in our statistical results might suggest the existence of a significant population of low-velocity impactors in early impact period (&gt;4Ga) around the cis-lunar space.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 106015"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142757209","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 estimate of resident time of the Oort Cloud new comets in planetary region","authors":"Takashi Ito ,&nbsp;Arika Higuchi","doi":"10.1016/j.pss.2024.105984","DOIUrl":"10.1016/j.pss.2024.105984","url":null,"abstract":"<div><div>We describe the result of our numerical orbit simulation which traces dynamical evolution of new comets coming from the Oort Cloud. We combine two dynamical models for this purpose. The first one is semi-analytic, and it models an evolving comet cloud under galactic tide and encounters with nearby stars. The second one numerically deals with planetary perturbation in the planetary region. Although our study does not include physical effects such as fading or disintegration of comets, we found that typical dynamical resident time of the comets in the planetary region is about <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>8</mn></mrow></msup></mrow></math></span> years. We also found that the so-called planet barrier works when the initial orbital inclination of the comets is small. A numerical result concerning the temporary transition of the comets into other small body populations such as transneptunian objects or Centaurs is discussed.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"253 ","pages":"Article 105984"},"PeriodicalIF":1.8,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142650870","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 ExoMars 2028 WISDOM antenna assembly: Description and characterization","authors":"Wolf-Stefan Benedix ,&nbsp;Sebastian Hegler ,&nbsp;Christoph Statz ,&nbsp;Ronny Hahnel ,&nbsp;Dirk Plettemeier ,&nbsp;Valérie Ciarletti","doi":"10.1016/j.pss.2024.105995","DOIUrl":"10.1016/j.pss.2024.105995","url":null,"abstract":"<div><div>While ground penetrating radars have been extensively researched on Earth, the high-resolution exploration and imaging of the shallow subsurface of celestial bodies in our solar system is still in its early stages, with only a handful of systems capable of the task.</div><div>Designing high-resolution radar systems can be a complex task due to the large frequency bandwidth required by the antennas to achieve high vertical resolution. The WISDOM GPR, as part of the 2028 ExoMars mission, is a highly capable and challenging instrument in this context, given its fully-polarimetric setup and mission constraints on the operating environment, robustness, as well as mass and size budget.</div><div>This paper outlines the development and characterization process of the WISDOM antenna assembly, which can serve as a model for future radar systems. Furthermore, it presents the results of the antenna characterization as the foundation for instrument calibration and optimal radar sounding outcomes.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"253 ","pages":"Article 105995"},"PeriodicalIF":1.8,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142650871","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":"Photogeological analysis of ShadowCam images of the permanently shadowed floor of lunar crater Shoemaker","authors":"А.T. Basilevsky ,&nbsp;S.S. Krasilnikov ,&nbsp;Yuan Li","doi":"10.1016/j.pss.2024.105998","DOIUrl":"10.1016/j.pss.2024.105998","url":null,"abstract":"<div><div>The photogeologic analysis of the ShadowCam images of the permanently shadowed floor and lower parts of inner slopes of the near-polar lunar crater Shoemaker confirmed the conclusion of Basilevsky and Li (2024)that the surface morphology of the Shoemaker floor is dominated by a population of small (D &lt; 1 km) craters. Future studies hopefully will allow to describe the morphology and morphometry (especially d/D) of the decameter-scale craters seen in the ShadowCam images. The surface of the lower parts of inners slopes of crater Shoemaker, which are permanently shadowed, has the “elephant hide” texture, that is also typical for normally illuminated slopes. So, most issues of the surface morphology were found to be identical or very close to those in normally illuminated regions of the Moon. The new finding in permanently shadowed areas is the presence of lobate-rimmed craters, whose morphology is probably indicative of water ice in the target material.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105998"},"PeriodicalIF":1.8,"publicationDate":"2024-11-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654042","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":"Performance evaluation of pansharpening for planetary exploration: A case study on the implementation of TGO CaSSIS with MRO HiRISE","authors":"A. Tullo ,&nbsp;C. Re ,&nbsp;G. Cremonese ,&nbsp;E. Martellato ,&nbsp;R. La Grassa ,&nbsp;N. Thomas","doi":"10.1016/j.pss.2024.105997","DOIUrl":"10.1016/j.pss.2024.105997","url":null,"abstract":"<div><div>The present study analyses the potential of pansharpening algorithms for planetary exploration studies, testing their performance with the 4-band images from the Colour and Stereo Surface Imaging System (CaSSIS) aboard the Exomars 2016 Trace Grace Orbiter (TGO) using HiRISE images from the Mars Reconnaissance Orbiter (MRO) mission as the base. Due to the lack of suitable open-source tools, a suite of scripts was developed to improve alignment between images and enable different component substitution (CS) pansharpening algorithms. The tools developed were tested on a database of images encompassing several regions of Mars to explore its vast diversity in colours, tones, and textures. Then, the resulting images were investigated using spectral and structural performance indices, comparing the results with the source images and the colour information from the HiRISE central channels.</div><div>The results show that a substantial number of the tested algorithms are more than suitable for data enhancement, showing a considerable improvement in the structural characteristics of the images without sacrificing their spectral characteristics. In detail, the Gram-Schmidt method, widely used in terrestrial pansharpening, turns out to be the best compromise among the tested algorithms. Regarding the other tested algorithms, GIHS and the MMSE Brovey, a modified version of the classic Brovey, show the most significant increase in structural properties, while GHPF and GHPM show the interesting ability to maintain virtually unchanged spectral conditions of the multispectral source data.</div><div>In addition, the analysis reveals the applicability of pansharpening at a ground resolution increment up to 18 times, from 4.5 up to 0.25 m/px, a broader range than is usually used in traditional pansharpening.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105997"},"PeriodicalIF":1.8,"publicationDate":"2024-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654041","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":"Formation of halotrichite in the South Kerala Sedimentary Basin, SW India: Implications for Martian paleo-environmental studies","authors":"Kannan J. Prakash ,&nbsp;Libiya M. Varghese ,&nbsp;P.B. Hiral ,&nbsp;Suresh Evna ,&nbsp;V.R. Rani ,&nbsp;K.S. Sajinkumar ,&nbsp;V.J. Rajesh ,&nbsp;G.K. Indu ,&nbsp;Sneha Mukherjee ,&nbsp;J.K. Tomson","doi":"10.1016/j.pss.2024.105999","DOIUrl":"10.1016/j.pss.2024.105999","url":null,"abstract":"<div><div>Halotrichite [FeAl₂(SO₄)₄·22(H₂O)] is a rare secondary sulfate mineral with its occurrence confined within the sulfide weathering zones. In the South Kerala Sedimentary Basin (SKSB) of SW India, halotrichite, here reported for the first time, is associated with an organic matter (OM)-rich carbonaceous clay layer. Field investigation revealed the prevalence of acid rock drainage (ARD) conditions similar to Martian analogue sites like Rio Tinto. The OM-layer is associated with pyrite forming substratum and Al-rich leachate associated with the Youngest Toba Tuff (YTT) cryptotephra layer. Oxidation of these units results in the formation of halotrichite, which is temporally restricted only to the dry season when the water table lowers and the OM-layer is exposed to air. X-Ray Diffraction (XRD) results for halotrichite show the presence of Al and Fe(II) sulfates. Energy Dispersive X-ray Spectroscopy (EDS) ruled out the existence of pickeringite, the Mg end-member of halotrichite-pickeringite series. XRD results for the OM-layer indicate the presence of kaolinite, quartz, goethite, and lepidocrocite. Hyperspectral analysis of the clay samples confirms that halotrichite is associated with goethite, lepidocrocite, kaolinite, and smectite. Fourier Transform Infrared Spectroscopy (FTIR) analysis revealed the major constituent of the clay sample as kaolinite with traces of quartz, smectite, and OM. Raman spectrum of halotrichite shows the symmetric stretching vibration of SO₄²⁻ bonded to Fe²⁺. Association of halotrichite with Fe, Al, and S-rich minerals is also inferred by the study of Raman spectrum of the host clay. Co-existence of halotrichite, goethite, lepidocrocite, and phyllosilicates in the study area is similar to the mineral assemblage found along the Rio Tinto River. On Mars, halotrichite is associated with the layered sulfate deposits, such as those in Valles Marineris and Meridiani Planum, and is categorized as a polyhydrated sulfate. Hence, this study on the halotrichite mineralization in the SKSB can supplement the attempts on deciphering the deposition and formation environment of similar mineralization on Mars.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105999"},"PeriodicalIF":1.8,"publicationDate":"2024-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654040","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":"Power attenuation of Martian rovers and landers solar panels due to dust deposition","authors":"Thomas Pierron,&nbsp;François Forget,&nbsp;Ehouarn Millour,&nbsp;Antoine Bierjon","doi":"10.1016/j.pss.2024.105985","DOIUrl":"10.1016/j.pss.2024.105985","url":null,"abstract":"<div><div>Because of the high amount of dust in the Martian atmosphere, solar panels of landers and rovers on Mars get covered by dust in the course of their mission. This accumulation significantly decreases the available power over sols. During some missions, winds were able to blow the dust away. These ”dust cleaning events”, as they are called, were followed by an increase of the electrical current produced by the solar arrays. However, the Insight Lander solar panels were never cleaned and the mission died of dust accumulation. In order to better predict the evolution of available power produced by solar panels in the Martian conditions, this paper proposes a model of dust accumulation in which the solar flux under the accumulated dust layer is computed taking into account a full radiative transfer in the atmosphere and in the dust layer accumulated on the panel. This work uses several missions observation data to validate this model.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"253 ","pages":"Article 105985"},"PeriodicalIF":1.8,"publicationDate":"2024-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142551898","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}