Icarus最新文献

{"title":"The blinking crystallinity of Europa: A competition between irradiation and thermal alteration","authors":"Cyril Mergny ,&nbsp;Frédéric Schmidt ,&nbsp;Félix Keil","doi":"10.1016/j.icarus.2025.116700","DOIUrl":"10.1016/j.icarus.2025.116700","url":null,"abstract":"<div><div>The surface of Europa experiences a competition between thermally-induced crystallization and radiation-induced amorphization processes, leading to changes of its crystalline structure. The non-linear crystallization and temperature-dependent amorphization rates, incorporating ions, electrons and UV doses, are integrated into our multiphysics surface model (MSM) <em>LunaIcy</em>, enabling simulations of these coupled processes on icy moons.</div><div>Thirty simulations spanning <span><math><mrow><mn>100</mn><mspace></mspace><mn>000</mn><mspace></mspace><mstyle><mi>y</mi><mi>e</mi><mi>a</mi><mi>r</mi><mi>s</mi></mstyle></mrow></math></span>, covering the full ranges of albedo and latitude values on Europa, explore the competition between crystallization and irradiation. This is the first modeling of depth-dependent crystallinity profiles on icy moons. The results of our simulations are coherent with existing spectroscopic studies of Europa, both methods showing a primarily amorphous phase at the surface, followed by a crystalline phase after the first millimeter depth. Our method provides quantitative insights into how various parameters found on Europa can influence the subsurface crystallinity profiles.</div><div>Interpolating upon our simulations, we have generated crystallinity maps of Europa showing highly crystalline ice near the equator, amorphous ice at the poles, and a mix of the two at mid-latitudes. Regions/depths with balanced competition between crystallization and amorphization rates are of high interest due to their periodic fluctuations in crystalline fraction. Our interpolated map reveals periodic variations, with seasonal amplitudes reaching up to 35% of crystalline fraction. These variations could be detected through spectroscopy, and we propose a plan to observe them in forthcoming missions.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116700"},"PeriodicalIF":2.5,"publicationDate":"2025-06-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144489759","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Phosphates reveal high pH ocean water on Enceladus","authors":"Christopher R. Glein,&nbsp;Ngoc Truong","doi":"10.1016/j.icarus.2025.116717","DOIUrl":"10.1016/j.icarus.2025.116717","url":null,"abstract":"<div><div>Enceladus offers our best opportunity for exploring the chemistry of an ocean on another world. Here, we perform geochemical modeling to show how the distribution of phosphate species found in ice grains from Enceladus's plume provides a very straightforward constraint on the pH of the host solution. The ratio of HPO₄/PO₄ species serves as a pH indicator. We find evidence of moderately alkaline water (pH 10.1–11.6)—significantly more alkaline than current estimates (∼8–9) of the pH of Enceladus's ocean. Nevertheless, the pH range from phosphates is consistent with the CO₂/H₂O ratio measured in the plume if CO₂ exsolves from ocean water according to its equilibrium solubility. A simple energy balance can be used to quantify volatile fractionation during gas transport inside Enceladus's tiger stripes; we deduce that ∼83 % of water vapor is removed as ice during transport between the liquid-vapor interface and where gases exit the subsurface. We also explore how CO₂ degassing may lead to an increase in the apparent pH of ocean water. We generate maps of allowed combinations of pH and dissolved inorganic carbon concentration of the source water for a wide range of scenarios. Our preferred interpretation, constrained by the observed heat flux, implies minimal CO₂ degassing from ocean water. Hence, the pH recorded by phosphates should closely approximate that of the ocean; our best estimate is pH ∼10.6. Such a high pH seems to reflect a major role of silicates enriched in Na, Mg, or Fe(II) interacting extensively with ocean water. Silica nanoparticles would not form or would subsequently dissolve if the pH is too high (&gt;10.5). The outgassing model presented here provides a new path to quantify the dissolved concentrations of volatile species.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116717"},"PeriodicalIF":2.5,"publicationDate":"2025-06-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144469912","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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 Amundsen-Ganswindt basin: An overlooked lunar peak-ring basin with multiple exploration opportunities","authors":"J. Hostrawser,&nbsp;G.R. Osinski","doi":"10.1016/j.icarus.2025.116718","DOIUrl":"10.1016/j.icarus.2025.116718","url":null,"abstract":"<div><div>The ∼ 355 km diameter Amundsen-Ganswindt impact basin (81°S, 120°E) has been stratigraphically constrained as the oldest large basin in the South Pole-Aitken basin terrane. It partly overlaps the Artemis Exploration Zone, across which it deposited significant volumes of impact ejecta deposits. The basin is highly degraded and partially superposed by the similar-sized Schrödinger peak-ring impact basin, leading previous workers to question whether it contains any remnants of an original peak-ring. We have conducted a detailed geologic study of the Amundsen-Ganswindt basin and evaluated the scientific potential of this ancient structure in the context of global lunar exploration objectives that underpin future crewed and robotic exploration missions to the lunar south polar region. We have mapped the basin at a scale of 1:1,000,000 and identified high-value exploration targets, including remnants of an original peak ring and opportunities to sample this uplifted material. Given its age, both Amundsen-Ganswindt's peak ring and ejecta deposits will contain a high proportion of material from the South Pole-Aitken basin. In addition, material from the Schrödinger peak-ring impact basin — the second youngest basin on the Moon — are also available for sampling. Morphological evidence suggests that the Amundsen-Ganswindt basin influenced the final morphology of Schrödinger's rim and peak ring. The Amundsen-Ganswindt basin is also host to large, accessible permanently shadowed regions with orbital detections of water ice. Thus, we propose that the overlooked Amundsen-Ganswindt basin is an exceptional exploration target for future robotic and human exploration missions.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116718"},"PeriodicalIF":2.5,"publicationDate":"2025-06-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144517824","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Transient and tidal wave precursors and atmospheric impacts of Mars’ flushing storm initiated regional storms in reanalysis data","authors":"Márton Mester ,&nbsp;R. John Wilson ,&nbsp;Melinda A. Kahre","doi":"10.1016/j.icarus.2025.116690","DOIUrl":"10.1016/j.icarus.2025.116690","url":null,"abstract":"<div><div>Regional dust storms develop in the Southern Hemisphere (SH) of Mars typically three times in years that do not experience a Global Dust Storm. The Thermal Emission Spectrometer and the Mars Climate Sounder instruments on board Mars Global Surveyor and Mars Reconnaissance Orbiter, respectively, have observed that the storms that generally appear in the <span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>s</mi></mrow></msub><mo>=</mo><mn>210</mn><mo>°</mo><mo>−</mo><mn>240</mn><mo>°</mo></mrow></math></span> and <span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>s</mi></mrow></msub><mo>=</mo><mn>310</mn><mo>°</mo><mo>−</mo><mn>330</mn><mo>°</mo></mrow></math></span> time periods, commonly referred to as A- and C-season regional dust storms, respectively, are preceded by atmospheric dust ‘flushed’ into the SH from the Northern Hemisphere (NH) mid-latitude storm track through one of the vast lowland channels, most frequently via Acidalia–Chryse or Utopia–Isidis. Here, reanalysis data are used to analyze the typical behavior of transient and tidal waves before and after cross-equator flushing storms that trigger regional storms, revealing the characteristic atmospheric wave evolution surrounding these events. In particular, the analysis shows that a strong wavenumber 3 transient wave and a mid-latitude tide amplification typically precede flushing events. Furthermore, our results suggest that while Acidalia-related regional storms typically require multiple high-amplitude wave events, regional storms initiated through Isidis may happen more abruptly.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116690"},"PeriodicalIF":2.5,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144489758","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Insights into pyroxene-dominated surfaces and implications for ongoing space exploration missions","authors":"B.G. Rider-Stokes ,&nbsp;E. Branagan-Harris ,&nbsp;K. Markus ,&nbsp;J.F. Snape ,&nbsp;S.L. Jackson ,&nbsp;S.S. Russell ,&nbsp;R.C. Greenwood ,&nbsp;T.H. Burbine ,&nbsp;M.J. Whitehouse ,&nbsp;D.A. Rothery ,&nbsp;L.F. White ,&nbsp;M.M. Grady","doi":"10.1016/j.icarus.2025.116713","DOIUrl":"10.1016/j.icarus.2025.116713","url":null,"abstract":"<div><div>Ungrouped achondrites are differentiated (melted) meteorites that do not fit into any known meteorite group because of their unusual mineralogies and/or oxygen isotopic compositions; their asteroidal or planetary origins are unknown. Two recently discovered samples, Northwest Africa 15915 (NWA 15915) and Ksar Ghilane 022 (KG 022), have mineral assemblages not previously identified in meteorites, consisting of iron-free silicates (including augite, enstatite, and olivine) and unusual sulphides (such as oldhamite). These samples offer the opportunity to probe the spectral properties of mineralogically distinct surfaces. NWA 15915 and KG 022 have oxygen isotopic compositions in the field of enstatite chondrites and aubrites, a near absence of spectral features in the visible and near-infrared, and a similar mineralogy to that which is expected for the surface of Mercury. While it is unlikely that the two meteorites are fragments of Mercury, they may be good analogs for Mercury's surface on a regional scale. ESA/JAXA's BepiColombo will provide an exceptional opportunity to compare the composition of differing mineralogical units on Mercury with samples such as NWA 15915 and KG 022.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116713"},"PeriodicalIF":2.5,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144330559","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Spectral reflectance (0.35–2.50 μm) properties of minerals and organic-bearing compounds exposed to current Martian surface conditions","authors":"S.A. Connell ,&nbsp;D.M. Applin ,&nbsp;E.A. Cloutis ,&nbsp;J.T. Poitras ,&nbsp;D.T. Dixon ,&nbsp;S.A. Mertzman ,&nbsp;P. Mann ,&nbsp;C. Royer ,&nbsp;T. Fornaro ,&nbsp;A. Broz ,&nbsp;R.C. Wiens","doi":"10.1016/j.icarus.2025.116712","DOIUrl":"10.1016/j.icarus.2025.116712","url":null,"abstract":"<div><div>Mars shows unambiguous evidence of once-abundant ancient liquid surface water, driving exploration of the planet to assess habitability and the possibility of life. The global martian surface has been studied using orbital and ground-based observations, revealing mineralogical diversity and widespread evidence of mineral hydration. However, how exactly these ancient, hydrated minerals are affected by the cold, dry, and desolate surface conditions of modern Mars remains poorly understood, which limits our understanding of their original hydration state. To better address Mars surface mineralogy, mineral detectability, and hydration state, we exposed a suite of 27 hydrous and anhydrous minerals and carbonaceous materials to Mars-like surface conditions for 66 days (∼500 Pa, CO₂, ambient temperature). The mineral phases included carbonates, halides, organics, oxides, phyllosilicates (micas and phyllosilicates), sulfates, sulfides, and zeolite. They were selected based on their relevance to past detection on Mars by remote sensing instruments and their importance for habitability and potential biosignatures. The minerals were periodically characterized with reflectance spectroscopy over the 0.35 to 2.50 μm wavelength region through a sealed sapphire glass window. Dehydration occurred for some, but not all, hydrated minerals, with decreased intensity of the hydration bands observed for halloysite, hectorite, illite, kaolinite, montmorillonite, nontronite, and trona. Our data indicated that dehydration can be gradual or abrupt, but none of our samples fully dehydrated, as the 1.90 μm absorption band persisted but became shallower in the seven samples that showed spectral changes. Hydroxyl (OH), as evidenced by a 1.40 μm region absorption feature and metal-OH absorption bands in the 2.00–2.50 μm region, was largely resistant to dehydroxylation under Mars-like surface conditions, with the exception of hectorite and trona. Data from this study is integral for the robust identification and interpretation of martian surface mineralogy observed by remote sensing instruments. The dehydration processes observed in this work suggest similar processes on Mars have likely occurred, which can affect spectroscopic mineral identification based on whether or not hydration absorption features are observed on both natural and abraded surfaces. Thus, this can have major implications for global estimates of the amount of ancient, mineral-bound water that is still present on the planet.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116712"},"PeriodicalIF":2.5,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144480727","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Chromium isotopes in CR chondrites reveal two distinct chondrule reservoirs","authors":"Aryavart Anand ,&nbsp;Klaus Mezger","doi":"10.1016/j.icarus.2025.116714","DOIUrl":"10.1016/j.icarus.2025.116714","url":null,"abstract":"<div><div>Chondrules, the dominant components of chondrites, provide crucial insights into early solar system formation and evolution. Due to the variability of Cr isotopes in the solar system, they can serve as powerful tracers of chondrule genealogy and the transport of precursor materials in the evolving solar disk. High-precision mass-independent Cr isotope data for individual chondrules from the CR chondrite Shişr 033 reveal a bimodal distribution of ε⁵⁴Cr that defines two isotopically distinct chondrule populations. The major population exhibits ε⁵⁴Cr values (∼1.3) consistent with prior analyses of CR chondrules, while a minor population has significantly lower ε⁵⁴Cr (∼0.8), overlapping with CV-CO-CM chondrules. This suggests chondrule migration across spatial gaps in the protoplanetary disk, likely from the CV-CO-CM reservoir to the CR sub-reservoir. Further, ⁵³Mn–⁵³Cr systematics indicate that Mn–Cr fractionation in CR chondrule precursors occurred ∼0.7 Ma after solar system formation, predating the primary CR chondrule formation event at ∼3.8 Ma, inferred from ²⁶Al–²⁶Mg, and ¹⁸²Hf–¹⁸²W chronometry of individual chondrules. These findings support a model in which secondary disk substructures, likely linked to early Jupiter growth, facilitated isotopic heterogeneities and material transport in the outer solar system. The presence of CV-CO-CM chondrules in CR chondrites further suggests outward material transport in the protoplanetary disk before CR parent body accretion. This study provides new constraints on chondrule formation, precursor evolution, and planetary disk dynamics.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116714"},"PeriodicalIF":2.5,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144501865","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Corrigendum to “Atmospheric response to high-resolution topographical and radiative forcings in a general circulation model of Venus: Time-mean structures of waves and variances” [Icarus 355 (2021) 114154]","authors":"Masaru Yamamoto ,&nbsp;Kohei Ikeda ,&nbsp;Masaaki Takahashi","doi":"10.1016/j.icarus.2025.116706","DOIUrl":"10.1016/j.icarus.2025.116706","url":null,"abstract":"","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116706"},"PeriodicalIF":2.5,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144306289","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Outcrop scale evidesnce of late-fluid flows and secondary sulfate minerals on exhumed surfaces – Earth versus Mars comparison","authors":"Ivy Ettenborough,&nbsp;Sara M. Shields,&nbsp;Anna Szynkiewicz","doi":"10.1016/j.icarus.2025.116711","DOIUrl":"10.1016/j.icarus.2025.116711","url":null,"abstract":"<div><div>Secondary sulfate minerals are abundant in Gale crater on Mars and in some cases exhibit distinctive morphological features on the exhumed surfaces of sedimentary formations. These are bright-toned sulfate-rich halos and salt accumulations on the eroded bedding planes, but their origin and aqueous processes are still not well understood. To address this knowledge gap, we investigated similar features of sulfate-rich deposits in the Rio Puerco watershed, New Mexico to better understand their formation processes. During five individual months between 2012 and 2024, the studied halo-like features, bedding planes, and pseudo-layers were enriched in various Ca-Mg-Na sulfate minerals such as gypsum, thenardite, bloedite and hexahydrite. These sulfate-rich accumulations were common at the outcrop scale on the exhumed surfaces of sedimentary rocks but in some years, they were also visible on aerial images. Comparisons between the individual wet and dry months suggest that their formation is directly controlled by episodic (ephemeral) water activity related to the semi-arid climate. Episodic flows and infiltration of meteoric water and repeated cycles of redissolution of the already existing sulfate-rich secondary minerals on and near the surface lead to their reprecipitation and distinctive accumulations in halo-like features, bedding planes, and pseudo-layers. We hypothesize that sulfate-rich halos and bedding planes observed in Gale crater on Mars might have been related to the late-stage fluid flows on or within the exhumed surfaces induced by past meteoric water activity under dry conditions.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116711"},"PeriodicalIF":2.5,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144339012","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Simulating the evolution of brine-saturated regolith on Mars","authors":"David Haack,&nbsp;Erika Kaufmann,&nbsp;Axel Hagermann","doi":"10.1016/j.icarus.2025.116691","DOIUrl":"10.1016/j.icarus.2025.116691","url":null,"abstract":"<div><div>We investigate the sublimation behaviour of brine-saturated Martian analogue materials in laboratory experiments and how compositional variations affect the development of the sample surfaces and subsurfaces. As a regolith analogue for our experiments, we used granular Saddleback basalt with the three grain size distributions 212–500 <span><math><mi>μ</mi></math></span>m, 212–2000 <span><math><mi>μ</mi></math></span>m, and 1000–2000 <span><math><mi>μ</mi></math></span>m. Our brine was composed of ferric sulphate, magnesium sulphate, and magnesium chloride. The samples were placed in a environmental chamber and exposed to a temperature of 243 K and a CO₂ atmosphere of 5 mbar for several days. The samples were then insolated at 590 W<!--> <!-->m⁻² with a solar simulator, representing the insolation rate at Mars whilst changes in surface morphology were monitored in vertical and lateral directions by two cameras. No explicit salt efflorescence could be produced on the surface. However, we found a stratification characterised by four layers developed within the samples. Beneath (i) a solidified crust at the surface, (ii) a dry, unconsolidated layer formed, partially characterised by white magnesium salt precipitates. A (iii) third layer was characterised by yellowish hydrated ferric sulphate precipitates, which filled considerable parts of the pore space between the regolith analogue grains. The (iv) fourth layer still contained water in the form of ice crystals and moisture. The spectral and mechanical properties of the sample surfaces were analysed after the sublimation experiment using reflectance spectroscopy in the visual and near/mid-infrared spectral range and cone penetration testing. The spectral comparisons of the uppermost crust with the non-saline regolith analogue material displayed a distinct spectral blue slope, indicating the presence of hydrated ferric sulfates. The strength of the upper crusts varied from marginally consolidated to strongly cemented depending on grain size and salt content. Our observations indicate that extensive salt crusts on the Martian surface are less likely to have been formed by brines present in the subsurface. Due to high evaporation rates, significant amounts of dissolved salts already precipitated below the surface of Mars, potentially leading to the formation of underground duricrusts.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"441 ","pages":"Article 116691"},"PeriodicalIF":2.5,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144489760","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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}