Planetary and Space Science最新文献_第5页

Thermal and electrochemical properties of a mixture of lunar regolith simulant (FJS-1) and CaF2 月球风化模拟物（FJS-1）和CaF2混合物的热电化学性质

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-07-16 DOI: 10.1016/j.pss.2025.106177

Yuta Suzuki , Seiya Tanaka , Takuya Goto

To establish the electrochemical reduction process of lunar regolith as an in-situ resource utilization technology on the Moon, it is crucial to prepare a high-temperature electrolytic melt that has a composition suitable for electrolysis. In this study, we propose a mixed melt consisting of lunar regolith, which comprises metal-oxide compounds, and CaF₂, which can be collected from fluorapatite on the Moon's surface. To characterize the lunar regolith-CaF₂ system, the thermal and electrochemical properties of a mixture of a lunar mare regolith simulant (FJS-1) and CaF₂ were investigated. The differential thermal analysis curves measured for various compositions of FJS-1 and CaF₂ found that the eutectic temperature was 1275 K at FJS-1:CaF₂ = 90:10 wt%, which is lower than the melting point of FJS-1, 1393 K. By electrochemical impedance spectroscopic technique, the electrical resistance of the melts at 1673 K was found to be 43 Ω for the FJS-1 melt, while the mixed melt of FJS-1 and CaF₂ (80:20 wt%) was found to be 5 Ω. The XRD analysis of the solidified melts revealed that the mixed melts' unique physical properties were due to the formation of chemical bonding of F⁻ ions due to CaF₂ and metal ions due to FJS-1. Furthermore, the electrochemical behavior of the mixed melt was investigated, demonstrating the electrodeposition of metals such as Si and Al derived from FJS-1. The reported data will provide new guidelines for designing electrolytic systems on the Moon, expanding the possibilities for controlling the temperature and electrochemical operations.

要将月壤的电化学还原过程建立为月球就地资源利用技术，关键是要制备一种具有适合电解成分的高温电解熔体。在这项研究中，我们提出了一种混合熔体，由月球风化层和CaF2组成，其中包括金属氧化物化合物，CaF2可以从月球表面的氟磷灰石中收集。为了表征月球风化层-CaF2体系，研究了月球风化层模拟物（FJS-1）和CaF2的混合物的热学和电化学性质。对FJS-1和CaF2的不同组分进行差热分析，FJS-1:CaF2 = 90:10 wt%时共晶温度为1275 K，低于FJS-1的熔点1393 K。通过电化学阻抗谱技术，FJS-1熔体在1673 K时的电阻为43 Ω，而FJS-1和CaF2的混合熔体（80:20 wt%）的电阻为5 Ω。对固化熔体的XRD分析表明，混合熔体具有独特的物理性能是由于CaF2与FJS-1形成了F−离子和金属离子的化学键。此外，对混合熔体的电化学行为进行了研究，证明了FJS-1衍生的Si和Al等金属的电沉积。报告的数据将为设计月球上的电解系统提供新的指导方针，扩大控制温度和电化学操作的可能性。

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引用次数: 0

On the formation of satellites in dense solid-particle disks 稠密固体颗粒盘中卫星的形成

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-07-18 DOI: 10.1016/j.pss.2025.106168

G. Madeira , L. Esteves , T.F.L.L. Pinheiro , P.V.S. Soares , N.S. Santos , B. Morgado

Single massive satellites are of great observational interest, as they can produce prominent and potentially detectable signatures. For terrestrial planets and super-Earths, giant impacts in the late stages of formation may generate dense self-gravitating disks — favourable environments for the formation of such satellites. Motivated by this, we explore satellite formation in dense solid-particle disks through three-dimensional N-body simulations, focusing on the effects of disk mass and the surface density exponent (

β

). Our results reveal significant variability in the masses and configurations of satellites formed under identical disk parameters, highlighting the stochastic nature of the process. Higher disk masses and flatter surface density profiles favour the formation of more massive satellites. Disks with masses above 0.03 planetary masses typically yield a single dominant satellite, while those between 0.003 and 0.03 tend to form two-satellite systems. On average, the mass of the largest satellite scales linearly with the initial disk mass, in agreement with analytical predictions. We estimate that a disk with a minimal mass of 0.03 planetary masses around a 1.6 Earth-mass planet orbiting a Sun-like star could form an Earth–Moon-like system detectable by telescopes with a photometric precision of 10 parts per million – a level achievable by the James Webb Space Telescope.

单个大质量卫星具有很大的观测价值，因为它们可以产生明显的、潜在的可探测信号。对于类地行星和超级地球，在形成后期的巨大撞击可能会产生致密的自引力盘——这是形成此类卫星的有利环境。受此启发，我们通过三维n体模拟研究了致密固体颗粒盘中卫星的形成，重点研究了盘质量和表面密度指数（β）的影响。我们的结果揭示了在相同的圆盘参数下形成的卫星的质量和结构的显著变化，突出了这一过程的随机性。更高的圆盘质量和更平坦的表面密度剖面有利于形成更大质量的卫星。质量超过0.03行星质量的圆盘通常会产生一个主要的卫星，而质量在0.003到0.03之间的圆盘往往会形成两个卫星系统。平均而言，最大卫星的质量与初始圆盘质量呈线性关系，这与分析预测一致。我们估计，一个最小质量为0.03行星质量的圆盘，围绕着一颗1.6地球质量的行星，围绕着一颗类似太阳的恒星运行，可以形成一个类似地月的系统，用望远镜可以探测到，光度精度为百万分之十——詹姆斯·韦伯太空望远镜可以达到这个水平。

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引用次数: 0

Demonstration of the low-temperature carbothermal process for producing oxygen from lunar regolith: Terrestrial test campaign 从月球风化层生产氧气的低温碳热过程的演示：陆地试验活动

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-06-30 DOI: 10.1016/j.pss.2025.106154

Alice Dottori , Ivan Troisi , Michèle Roberta Lavagna

The solid-gas carbothermal reduction is one of the processes available for extracting oxygen from the lunar regolith, a crucial capability for supporting lunar exploration and establishing a sustainable human presence on the Moon’s surface. This article presents the findings of the experimental campaign conducted at the Politecnico di Milano, which confirmed the feasibility of the process. Water is extracted from dry regolith, and the production of carbon oxides is monitored to gather data on the process. The campaign studied the influence of various parameters to enhance water and oxygen production, including reaction temperatures, regolith granularity and mass, solid-to-gas ratio, processing duration, and others. The extracted water is collected in a condensation stage, while the evolution of the gaseous mixture is monitored using gas chromatography, and the exhaust batch of simulant is analysed through SEM and XRD. These analyses provided qualitative and quantitative assessments of the reaction’s effectiveness, yielding important information about the impact of changing parameters. The study concludes by proposing a set of process parameters to serve as a baseline for future implementation of the low-temperature carbothermal process on the lunar surface.

固体-气体碳热还原是从月球风化层中提取氧气的一种方法，这是支持月球探测和在月球表面建立可持续人类存在的关键能力。本文介绍了在米兰理工大学进行的实验活动的结果，证实了该过程的可行性。从干燥的风化层中提取水，并监测碳氧化物的产生，以收集有关该过程的数据。该活动研究了各种参数对提高水和氧产量的影响，包括反应温度、风化层粒度和质量、固气比、处理时间等。在冷凝阶段收集提取的水，同时使用气相色谱法监测气体混合物的演变，并通过SEM和XRD分析模拟物的排气批次。这些分析提供了反应有效性的定性和定量评估，提供了关于参数变化影响的重要信息。该研究最后提出了一套工艺参数，作为未来在月球表面实施低温碳热过程的基线。

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引用次数: 0

On the directional nature of the fall of celestial objects on the surface of Venus 论天体落在金星表面的方向性

IF 1.7 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-07-23 DOI: 10.1016/j.pss.2025.106167

Debashis Chatterjee , Prithwish Ghosh

This study demonstrates the critical need for circular data analysis in interpreting meteor impact locations on Venus. Traditional linear methods need to be improved to capture the cyclic nature of these data. We can better identify patterns and trends using specialized circular data techniques, enhancing our understanding of the mechanisms behind meteor impacts. By employing specialized statistical techniques that capture the cyclic nature of angular data, our analysis included Watson’s test at a 0.05 significance level, showing that the Venus surface crater dataset’s location parameters and solar elevations conform to a Von Mises distribution, while daytime and nighttime solar elevations do not. Using Bayesian Information Criterion (BIC) scores, we also determine that a two-component mixture of Fisher–von Mises distributions best models the spatial distribution of impact craters. These findings enhance our understanding of meteor impact processes on Venus and highlight the advantages of applying maximum-entropy directional models to planetary science.

这项研究表明，在解释金星上流星撞击位置时，对圆形数据分析的迫切需要。传统的线性方法需要改进，以捕捉这些数据的循环特性。我们可以使用专门的循环数据技术更好地识别模式和趋势，增强我们对流星撞击背后机制的理解。通过采用专门的统计技术捕捉角度数据的周期性，我们的分析包括0.05显著性水平的沃森检验，表明金星表面陨石坑数据集的位置参数和太阳高度符合冯米塞斯分布，而白天和夜间太阳高度则不符合。利用贝叶斯信息准则（BIC）得分，我们还确定了Fisher-von Mises分布的双组分混合最能模拟陨石坑的空间分布。这些发现增强了我们对金星流星撞击过程的理解，并突出了将最大熵方向模型应用于行星科学的优势。

引用次数: 0

Water-group ion irradiation studies of Enceladus ice analogues: Can radiolysis account for material in and around the south polar plume? 土卫二冰类似物的水基离子辐射研究：辐射分解能解释南极羽流内部和周围的物质吗？

IF 1.7 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-07-19 DOI: 10.1016/j.pss.2025.106179

Grace Richards , Richárd Rácz , Sándor T.S. Kovács , Victoria Pearson , Geraint Morgan , Manish R. Patel , Simon Sheridan , Duncan V. Mifsud , Béla Sulik , Sándor Biri , Nigel J. Mason , Robert W. McCullough , Zoltán Juhász

Saturn's magnetosphere contains trapped plasma and energetic charged particles which constantly irradiate the surface of Enceladus. In this study, we exposed Enceladean surface ice analogues containing H₂O, CO₂, CH₄, and NH₃ to water-group ions (e.g., O⁺, O³⁺, OH⁺, and H₂O⁺) having energies between 10 and 45 keV with the aim of exploring the chemical evolution of these ices and characterising the extent to which the surface material on Enceladus is weathered by Saturn's radiation environment. Each irradiation process was monitored in situ using Fourier-transform mid-infrared transmission absorption spectroscopy, and post-irradiative warming of the ices was performed to better characterise complex organic molecules formed as a result of the mobilisation of radiolytically generated radicals. Irradiation resulted in the formation of CO, OCN⁻, and NH₄⁺ in all experiments, and the radiolytic formation of formamide, acetylene, acetaldehyde, and hydroxymethyl radicals was also tentatively suggested in most experiments. Post-irradiative warming of the ices resulted in the formation of carbamic acid, ammonium carbamate, and an alcohol species. Although many of these products have not been previously observed on Enceladus' surface, some have been detected in Enceladus' plumes. Since our results demonstrate that the radiolytic formation of these molecules can occur over timescales similar to the exposure times of plume and surface material to magnetospheric radiation, questions must be raised as to whether such material originates directly from the subsurface ocean or is instead formed within the radiation-rich space environment.

土星的磁层包含被捕获的等离子体和高能带电粒子，它们不断照射着土卫二的表面。在这项研究中，我们将土卫二表面含有H2O、CO2、CH4和NH3的类似冰暴露于能量在10到45 keV之间的水基离子（如O+、O3+、OH+和H2O+）中，目的是探索这些冰的化学演化，并表征土卫二表面物质被土星辐射环境风化的程度。利用傅里叶变换中红外透射吸收光谱对每个辐照过程进行现场监测，并对冰进行辐照后的加热，以更好地表征由于辐射分解产生的自由基的动员而形成的复杂有机分子。在所有的实验中，辐射都导致CO、OCN−和NH4+的形成，并且在大多数实验中也初步提出了甲酰胺、乙炔、乙醛和羟甲基自由基的辐射分解形成。辐照后的冰变暖导致氨基甲酸、氨基甲酸铵和一种醇的形成。虽然这些产物中的许多以前没有在土卫二表面观察到，但有些已经在土卫二的羽流中被检测到。由于我们的研究结果表明，这些分子的辐射分解形成可能发生在与羽流和表面物质暴露于磁层辐射的时间尺度相似的时间尺度上，因此必须提出这样的问题，即这些物质是直接来自地下海洋还是在富含辐射的空间环境中形成的。

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引用次数: 0

A shocked lithic clast with compositionally contrasting melt domains in the impact melt breccia-a first report from the Dhala impact structure, India 撞击熔融角砾岩中具有组成对比的熔融域的冲击岩屑——来自印度达拉撞击构造的第一份报告

IF 1.7 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-07-22 DOI: 10.1016/j.pss.2025.106180

Jayanta Kumar Pati , Anuj Kumar Singh , Shivanshu Dwivedi

Bolide impacts are associated with enormous amount of kinetic energy which transforms into humongous shock pressures (∼100 GPa) and temperatures (up to 20,000 °C) on the planetary surfaces. These extreme conditions result in unique shock features that are routinely used as diagnostic evidence to confirm the meteorite impact origin of a structure. Occurrence of diaplectic glass pseudomorphing various minerals is one of the unequivocal evidences of shock metamorphism. Similarly, complete rock melting requires pressure in the excess of 60 GPa; however, the melting processes are not well constrained and remain ambiguous. The present study focuses on shock-induced melting of a quartzo-feldspathic lithic clast within an impact melt breccia sample from the Dhala structure, India. Multiple felsic melt stringers and a silicic melt (similar to lechatelierite) lense were observed across the clast, displaying a linear mixing trend between K-feldspar and silica. The occurrences of planar deformation features in quartz, melt clasts, spherules, and traces of coesite indicate characteristics of shock metamorphism. The presence of coesite (a high-pressure silica polymorph), formed during shock pressure release from the silica melt, was verified through Raman spectroscopy. Compositions of felsic melt stringers seem to mimic eutectic melting similar to a synthetic K₂O-Al₂O₃-SiO₂ system suggesting the dominant role of eutectic type punctuated melting rather than instantaneous melt behaviour. This pattern contrasts with an immediate, widespread melting often reported in impactites worldwide.

火流星撞击与巨大的动能有关，这些动能在行星表面转化为巨大的冲击压力（~ 100 GPa）和温度（高达20,000°C）。这些极端条件导致了独特的冲击特征，这些特征通常被用作诊断证据，以确认一个结构的陨石撞击起源。各种矿物中出现偏射玻璃伪晶是冲击变质作用的明确证据之一。同样，岩石完全熔化需要超过60gpa的压力；然而，熔融过程没有得到很好的约束，仍然是模糊的。目前的研究主要集中在印度达拉构造的冲击熔融角砾岩样品中的石英长石岩屑的冲击诱导熔融。在岩屑中观察到多个长石熔体条纹和一个类似于光长石的硅熔体透镜，显示出钾长石与二氧化硅的线性混合趋势。石英、熔体碎屑、球粒的平面变形特征及钴矿的痕迹显示了冲击变质的特征。通过拉曼光谱验证了硅熔体在冲击压力释放过程中形成的硅矿（一种高压硅多晶）的存在。长硅熔体串的组成似乎模拟了类似于合成K2O-Al2O3-SiO2体系的共晶熔化，表明共晶间断熔化的主导作用，而不是瞬时熔化行为。这种模式与在世界各地的撞击中经常报道的立即、广泛的融化形成对比。

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引用次数: 0

Experimental investigation of solar radiation effects on Mercury’s surface regolith 太阳辐射对水星表面风化层影响的实验研究

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-15 Epub Date: 2025-07-17 DOI: 10.1016/j.pss.2025.106166

Nicole Latsia , Georgios Tsirvoulis , Erika Kaufmann , David Haack , Mikael Granvik , Axel Hagermann

The surface of Mercury is exposed to extreme diurnal thermal variations caused by the high intensity of solar radiation, the radiative loss due to the planet’s lack of atmosphere, its eccentricity and its 3:2 spin - orbit resonance. This work presents an experimental study on terrestrial rocks used as Mercury analogues subjected to hermean conditions. We simulate the power density of a planetary surface at Mercury’s perihelion distance of 0.31 au using the Space and High-Irradiance Near-Sun Simulator (SHINeS) at Luleå University of Technology. The reflectance spectra were acquired in the visible and near-infrared wavelength range for every sample before and after irradiation. Permanent spectral changes are observed in all samples towards the longer wavelengths in the visible spectrum after only one thermal cycle. Darkening is evident in both the visible and near-infrared spectrum ranges, combined with reddening in the visible-to-near-infrared region in most of our samples. We propose that darker samples like boninite, basalt, and diorite are more likely to experience spectral changes due to their low albedo.

水星表面暴露在极端的日热变化中，这是由高强度的太阳辐射、由于地球缺乏大气层而造成的辐射损失、它的偏心和3:2的自旋轨道共振造成的。这项工作提出了一项实验研究，用于地球岩石作为水星类似物受到她的平均条件。我们利用吕勒堡理工大学的空间和高辐照度近太阳模拟器（shine）模拟了水星近日点距离为0.31 au的行星表面的功率密度。获得了辐照前后样品在可见光和近红外波段的反射光谱。经过一个热循环后，所有样品的可见光谱都向着较长波方向发生了永久性的光谱变化。在可见和近红外光谱范围内，变暗是明显的，在我们的大多数样品中，在可见到近红外区域结合变红。我们提出，较暗的样品，如博宁岩、玄武岩和闪长岩，由于它们的低反照率，更有可能经历光谱变化。

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引用次数: 0

Seismic wave experiments in granular media with applications to asteroids 颗粒介质中的地震波实验及其在小行星上的应用

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-01 Epub Date: 2025-06-30 DOI: 10.1016/j.pss.2025.106153

Thomas Gallot, Camila Sedofeito, Alejandro Ginares, Gonzalo Tancredi

Observational data support the view of asteroids as granular systems. Characterizing their mechanical properties is crucial for space mission planning, assessing Earth’s impact risks, and understanding solar system origins. In this context, we present a laboratory-scale experiment aimed at examining wave propagation in granular media. Our findings demonstrate that the propagation of observed waves at 500 Hz shows significant attenuation with an estimated value of

α = (1.8 \pm 0.2)

Np/m. Additionally, we observe an increase in wave speed with confining pressure, which follows a dependency on

p^{1 / 2}

, interpreted as mesoscopic nonlinear elasticity. This indicates that a confined granular medium behaves as a nonlinear consolidated medium. Furthermore, we establish the equivalence of propagation properties between impact and vibration by supporting our experimental data analysis with numerical simulations. Applying our findings to model wave propagation in a low-gravity setting involving Dimorphos’ mass and geometry, our laboratory-based approach offers a cost-effective alternative to in situ measurements.

观测数据支持小行星是颗粒系统的观点。描述它们的机械特性对于空间任务规划、评估地球撞击风险和了解太阳系起源至关重要。在这种情况下，我们提出了一个实验室规模的实验，旨在检查波在颗粒介质中的传播。我们的研究结果表明，在500 Hz下，观测波的传播表现出明显的衰减，估计值为α=(1.8±0.2)Np/m。此外，我们观察到波速随围压的增加而增加，这取决于p1/2，这被解释为介观非线性弹性。这表明受约束的颗粒介质表现为非线性固结介质。此外，我们通过数值模拟来支持我们的实验数据分析，建立了冲击和振动之间的等效传播特性。将我们的研究结果应用于低重力环境下涉及Dimorphos质量和几何形状的波传播模型，我们基于实验室的方法为原位测量提供了一种经济有效的替代方法。

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引用次数: 0

A composite phase function for cometary dust comae 彗星尘埃彗星的复合相函数

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-01 Epub Date: 2025-07-07 DOI: 10.1016/j.pss.2025.106164

Ivano Bertini , Jean–Baptiste Vincent , Raphael Marschall , Fiorangela La Forgia , Alessandra Mura , Laura Inno , Stavro Ivanovski , Michael Küppers , Cecilia Tubiana , Vladimir Zakharov

Comets represent the most preserved planetesimals we can nowadays study and dust is one of their major components. Once emitted in the coma, cometary dust particles represent anisotropic scatterers of the incident solar light and their nature can be investigated with remote sensing studies. Among them, the measurement of the phase function curve has a key importance in several scientific aspects. It can be inverted with theoretical and laboratory studies to derive hints on the intimate nature of the emitted dust. It is also needed in adjusting cometary dust production rates for phase angle effects when data obtained throughout large time intervals are correlated. Finally, it is useful for space instruments planning since it provides inputs for optimal exposure times for remote sensing sensors which observe the coma spanning a large range of phase angles during close approaches. This will be particularly valuable in the framework of the future ESA Comet Interceptor mission which is going to fly-by a Dynamically New Comet entering our Inner Solar System for the very first time, carrying instruments which will image the coma with different observing geometries and phase angles in a short amount of time. In order to provide an useful tool to address the aforementioned scientific topics, we used available literature data to build a new composite phase function for cometary dust comae. This was obtained fitting Henyey–Greenstein functions to the original data of 11 comets and then connecting them in a continuous way as all data values were coming from a single average comet. We then fitted our result with a compound Henyey–Greenstein curve and compared it with previous models which were not including recent literature data constituting fine follow-ups of comets at small and large phase angles. The main difference is found in the description of the forward scattering surge, where our model depicts intensity one order of magnitude larger than previous ones. This finding is extremely important since it shows that the choice of the model may have severe consequences when interpreting, or instrumentally planning, forward scattering data.

彗星代表了我们现在可以研究的保存最完好的星子，尘埃是它们的主要组成部分之一。一旦在彗发中发射，彗星尘埃颗粒代表入射太阳光线的各向异性散射体，它们的性质可以通过遥感研究来研究。其中，相函数曲线的测量在若干科学领域具有重要意义。它可以通过理论和实验室研究来反转，以获得关于发射尘埃的亲密性质的提示。当在大时间间隔内获得的数据相互关联时，还需要调整相角效应的彗星尘埃产生率。最后，它对空间仪器规划很有用，因为它为遥感传感器在近距离接近时观测跨越大范围相位角的彗发提供了最佳曝光时间的输入。这将在未来ESA彗星拦截器任务的框架内特别有价值，该任务将飞越一颗首次进入我们内太阳系的动态新彗星，携带仪器将在短时间内以不同的观测几何形状和相位角对彗发进行成像。为了提供一个有用的工具来解决上述科学问题，我们利用现有的文献数据建立了一个新的彗星尘埃彗发的复合相位函数。这是将heney - greenstein函数拟合到11颗彗星的原始数据中，然后以连续的方式将它们连接起来，因为所有的数据值都来自一颗平均彗星。然后，我们用复合heney - greenstein曲线拟合我们的结果，并将其与之前的模型进行比较，这些模型不包括最近的文献数据，这些数据构成了彗星在小相角和大相角的精细后续。主要的区别在于对前向散射浪涌的描述，我们的模型描述的强度比以前的模型大一个数量级。这一发现非常重要，因为它表明，模型的选择可能会在解释或仪器规划前向散射数据时产生严重后果。

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引用次数: 0

A sliding window method considering image shadow to detect Mars rock from MRO HiRISE datasets 一种考虑图像阴影的滑动窗口方法用于MRO HiRISE数据集的火星岩石探测

IF 1.8 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Planetary and Space Science

Pub Date : 2025-10-01 Epub Date: 2025-06-21 DOI: 10.1016/j.pss.2025.106155

Na Sun , Yongjiu Feng , Xiaohua Tong , Pengshuo Li , Rong Wang , Yuhao Wang , Yuze Cao , Zilong Cao , Xiong Xu , Yusheng Xu , Shijie Liu

Rock distribution is a crucial factor in landing site selection for Mars exploration. Typically, rocks in flat Martian terrains are characterized by clear boundaries and distinct shadows. We developed a new method (named SSW-ROCK) for rock detection from HiRISE images using the shadow (S) and sliding window technique (SW). SSW-ROCK uses shadows to define the minimum bounding rectangle in the direction of illumination, establishing an initial sliding window based on this rectangle. The window is then slid to the termination position according to the predefined conditions. The rock size can be obtained by fitting the ellipse with the positions of the initial and termination windows. The rock height is estimated using the shadow length along the illumination direction. We used five HiRISE images of Mars between 65° N −70° N for rock detection and detected 532,284 rocks with maximum diameters >1.5 m. We selected accuracy assessment areas in each of the five images and extracted the rocks manually. The SSW-ROCK results were assessed for accuracy using the manual results as a benchmark. In the assessment, we proposed two evaluation metrics, PS and PM: PS measures the proportion of SSW-ROCK results with center points within the range of manual results, while PM measures the proportion of manual results with center points within the range of SSW-ROCK results. Accuracy assessments in five selected areas showed that the mean for both PS and PM exceeded 77 %. Additionally, the dimensions detected by the SSW-ROCK method for known Mars landers closely match their actual sizes. These experiments demonstrate that the SSW-ROCK method is effective for rock detection in flat Martian terrains.

岩石分布是火星探测着陆点选择的关键因素。通常，火星平坦地形上的岩石具有清晰的边界和明显的阴影。我们开发了一种利用阴影(S)和滑动窗口技术（SW）从HiRISE图像中检测岩石的新方法（命名为SSW-ROCK）。SSW-ROCK使用阴影来定义光照方向上的最小边界矩形，并在此矩形的基础上建立一个初始滑动窗口。然后根据预定义的条件将窗口滑动到终止位置。岩石尺寸可以通过椭圆与初始和终止窗口的位置拟合得到。利用沿光照方向的阴影长度估计岩石高度。我们使用了5张位于65°N - 70°N之间的火星HiRISE图像进行岩石检测，共检测到532,284块岩石，最大直径为1.5 m。我们在每张图像中选择精度评估区域，并手动提取岩石。使用手动结果作为基准评估SSW-ROCK结果的准确性。在评价中，我们提出了两个评价指标PS和PM: PS衡量的是SSW-ROCK结果中点在人工结果范围内的比例，PM衡量的是SSW-ROCK结果中点在人工结果范围内的比例。五个选定地区的准确性评估表明，PS和PM的平均值均超过77%。此外，SSW-ROCK方法探测到的已知火星着陆器的尺寸与它们的实际尺寸非常接近。实验结果表明，SSW-ROCK方法对于火星平坦地形的岩石探测是有效的。

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