Solar System Research最新文献

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An Optically Thin and Thick Dust Exosphere of Active Asteroids: Spectral Signs and Possible Formation Mechanisms 活跃小行星的光学薄厚尘埃外层：光谱迹象和可能的形成机制

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/S003809462470014X

V. Busarev, E. V. Petrova, V. Puzin, S. Barabanov, M. Shcherbina, S. Y. Kuznetsov

引用次数: 0

Crater Formed by the Impact of the Luna-25 Spacecraft 月球-25 号飞船撞击形成的陨石坑

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/s0038094623700090

A. T. Basilevsky, B. A. Ivanov, V. P. Dolgopolov

Abstract

On August 11, 2023, the Luna-25 spacecraft was launched with the task of landing in the southern polar region of the Moon and conducting research on the soil and near-surface exosphere. It flew safely to the Moon vicinity and settled into the orbit of Moon satellite. The landing of the spacecraft was scheduled for August 21. In accordance with the flight program, on August 19, a braking impulse was issued to form a pre-landing orbit. But the braking engine worked longer than planned, and the spacecraft crashed into the lunar surface. The team of the LROC television camera of the Lunar Reconnaissance Orbiter, having received information from Roscosmos about the crash site of Luna-25, photographed this site and on August 24 received an image showing a morphologically fresh crater with a diameter of about 10 m, which was not present in previous images of this site. The paper describes the regional topographic and geological characteristics of the site. A photogeological analysis of LROC images of the impact site was performed. An estimate has been made of the expected diameter of the crater formed as a result of the impact of Luna-25. From our examination, it follows that the 10-meter crater described in the NASA message appears to have actually been formed as a result of the impact of Luna-25. Its size corresponds to estimates calculated from impact parameters. The absence of a bright halo of emissions, typical of very young lunar craters, is likely due to the fact that the impact was relatively low-velocity, and in this case the crater is more likely an indentation depression and/or due to the fact that there was about half a ton of unspent fuel in the spacecraft “smeared” the surface near the crater.

摘要 2023 年 8 月 11 日，月球-25 号航天器发射升空，其任务是在月球南极地区着陆并对土壤和近地表外大气层进行研究。它安全飞抵月球附近，并进入月球卫星轨道。飞船计划于 8 月 21 日着陆。按照飞行计划，8 月 19 日，飞船发出制动脉冲，形成着陆前轨道。但制动发动机的工作时间超过了计划，飞船坠入了月球表面。月球勘测轨道飞行器的 LROC 电视摄像机小组从俄罗斯航天局获得了有关月球-25 号坠毁地点的信息，对该地点进行了拍摄，并于 8 月 24 日获得了一张显示一个形态新颖、直径约 10 米的陨石坑的图像，这在该地点以前的图像中是没有的。论文介绍了该地点的区域地形和地质特征。对该撞击点的 LROC 图像进行了光地质学分析。对月球-25 撞击形成的陨石坑的预期直径进行了估计。根据我们的研究，NASA 信息中描述的 10 米陨石坑似乎确实是月球-25 撞击形成的。它的大小与根据撞击参数计算出的估计值相符。由于撞击的速度相对较低，在这种情况下，陨石坑更可能是一个凹陷洼地和/或由于航天器中约有半吨未用完的燃料 "涂抹 "在陨石坑附近的表面上，所以没有出现非常年轻的月球陨石坑所特有的明亮的放射光晕。

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引用次数: 0

Impact Structures on Venus as a Result of Asteroid Destruction in the Atmosphere 小行星在大气层中的破坏导致金星上的撞击结构

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/s0038094623700089

V. V. Shuvalov, B. A. Ivanov

Abstract—

Venus’ thick atmosphere is capable of destroying kilometer-sized bodies such as asteroids, creating various types of traces on the surface. While larger cosmic bodies are able to reach the surface, creating impact craters or crater dispersion fields, smaller bodies effectively transfer the initial kinetic energy into the atmosphere, resulting in an “atmospheric explosion” at some altitude. In these cases, the most visible marks on the surface of Venus are created by atmospheric shock waves and the flow of gas behind the shock fronts reflected from the solid surface. The transitional sizes of impactors that break up in the atmosphere but reach the surface give rise to clusters of craters. The paper presents the first results of three-dimensional calculations of the destruction of rocky asteroids in the atmosphere of Venus, indicating significant differences from simple two-dimensional axisymmetric calculations.

摘要--金星厚厚的大气层能够摧毁小行星等千米大小的天体，在表面形成各种痕迹。较大的宇宙天体能够到达地表，形成撞击坑或陨石坑扩散场，而较小的天体则能有效地将初始动能转移到大气层中，在一定高度形成 "大气爆炸"。在这些情况下，金星表面上最明显的痕迹是由大气冲击波和冲击波前沿后方的气体流从固体表面反射造成的。在大气层中碎裂但到达地表的撞击物的过渡尺寸会产生陨石坑群。论文首次提出了金星大气层中岩质小行星破坏的三维计算结果，表明与简单的二维轴对称计算有显著差异。

引用次数: 0

Radiolysis as a Possible Mechanism for Perchlorate Synthesis on Mars and Europa 辐射分解是火星和欧罗巴上高氯酸盐合成的可能机制

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/s0038094624700126

D. V. Belousov, V. S. Cheptsov, A. K. Pavlov

Abstract—

Perchlorates have been found in the regolith of Mars and the Moon, in the ice of Europa, and in meteorites. Studying the processes of formation and destruction of these compounds is important both for understanding the geological and climatic evolution of a number of planets and bodies of the Solar System, and for assessing their habitability. To date, a number of processes for the synthesis of perchlorates under Martian conditions have been proposed, but these do not explain the perchlorate concentrations observed in the regolith and are not applicable to atmosphereless bodies, in particular Europa. We have studied the processes of synthesis and destruction of perchlorates during irradiation of ice and regolith models with high-energy electrons under conditions of low temperature (–50°C) and in the absence of an atmosphere (at a pressure of 0.01 mbar). The data obtained indicate that perchlorates can be efficiently synthesized in the regolith of Mars and the surface layer of Europa ice under the influence of irradiation in the absence of a liquid phase or an atmosphere.

摘要-在火星和月球的碎屑岩、欧罗巴冰层以及陨石中都发现了高氯酸盐。研究这些化合物的形成和破坏过程对于了解一些行星和太阳系天体的地质和气候演变以及评估它们的宜居性都非常重要。迄今为止，已经提出了一些在火星条件下合成高氯酸盐的过程，但这些过程无法解释在碎屑岩中观测到的高氯酸盐浓度，也不适用于无大气层的天体，特别是木卫二。我们研究了在低温（-50°C）和无大气（压力为 0.01 毫巴）条件下，用高能电子辐照冰和碎屑模型时高氯酸盐的合成和破坏过程。所获得的数据表明，在没有液相或大气的情况下，在辐照的影响下，可以在火星的碎石和欧罗巴冰的表层有效地合成高氯酸盐。

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引用次数: 0

Obtaining Plasma–Dust Clouds from Meteoritic Matter, its Analogs and Simulants of Lunar Regolith Using Microwave Discharge 利用微波放电从陨石物质、其类似物和月球碎屑模拟物中获取等离子尘云

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700138

V. Borzosekov, N. Akhmadullina, A. S. Sokolov, T. E. Gayanova, A. D. Rezaeva, V. Stepakhin, E. M. Konchekov, D. Malakhov, E. V. Voronova, I. R. Nugaev, V. Logvinenko, A. V. Knyazev, A. A. Letunov, D. E. Kharlachev, E. A. Obraztsova, T. I. Morozova, M. A. Zaitsev, A. V. Ishchenko, I. A. Weinstein, V. Grohovsky, O. Shishilov, N. Skvortsova

引用次数: 0

Features of Space Debris Migration in the Earth–Moon System 地月系统中空间碎片迁移的特点

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700199

T. Salnikova, E. Kugushev

引用次数: 0

Potentially Primary Xenon Components in Nanodiamond-Enriched Meteorite Fractions: New Isotopic Compositions and Carrier Phases 富含纳米金刚石的陨石碎片中潜在的原生氙成分：新同位素组成和载体相

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/s0038094623700065

A. V. Fisenko, L. F. Semenova, T. A. Pavlova

Abstract—

The potential primary component composition of xenon in nanodiamond-enriched fractions (NDFs) of meteorites was determined under the assumption that it contains two almost normal, but different isotopic components (Xe-P3 and Xe-P3n). The Xe-P3n component is contained in the individual population of diamond grains, while the Xe-P3 component is contained in diamond-like rims on the diamond grains. The presence of the Xe-P3n component made it possible to use radioactive products of the classical r-process of nucleosynthesis during a type II supernova explosion to form, according to the hypothesis of Ott (1996), two xenon components with an anomalous isotopic composition (Xe-pr1n and Xe-pr2n) without an increased isotope content of ¹³²Xe relative to the isotope content of ¹³⁶Xe. It is assumed that the implantation (sorption) of isotopes of the Xe-pr1n and Xe-pr2n components into their carrier phases probably occurred in turbulent mixing zones of different compositions in the outer and inner shells of a type II supernova after its explosion. The Xe-pr1n component is contained in an individual population of nanodiamond grains, while the Xe-pr2n carrier phase is first suggested to be SiC-X grains, the evolution of which is associated with a type II supernova. Therefore, when SiC-X grains are destroyed, for example, under laboratory conditions, a mixture of Xe-S and Xe-pr2n components is released, which we denote as Xe-X. Thus, according to the concept we proposed, the primary component composition of xenon consists, in addition to Xe-S, of Xe-P3, Xe-P3n, Xe-pr1n and Xe-X, contained in different individual carrier phases. Successful calculations of the abundances of these components in the NDF of such different meteorites as Murchison CM2 and Allende CV3 and their analysis have shown that the above components may be real components.

摘要-陨石的纳米金刚石富集馏分（NDFs）中氙的潜在主要成分组成是根据它包含两个几乎正常但不同的同位素成分（Xe-P3 和 Xe-P3n）这一假设确定的。Xe-P3n 成分包含在金刚石晶粒的个体中，而 Xe-P3 成分则包含在金刚石晶粒的金刚石状边缘中。根据 Ott（1996 年）的假设，Xe-P3n 成分的存在使得利用 II 型超新星爆炸期间核合成经典 r 过程的放射性产物来形成两个同位素组成异常的氙成分（Xe-pr1n 和 Xe-pr2n）成为可能，但 132Xe 的同位素含量相对于 136Xe 的同位素含量并没有增加。据推测，Xe-pr1n 和 Xe-pr2n 成分的同位素植入（吸附）到它们的载体相中，很可能发生在 II 型超新星爆炸后其外壳和内壳中不同成分的湍流混合区。Xe-pr1n成分包含在纳米金刚石晶粒的个体群中，而Xe-pr2n载相则首先被认为是SiC-X晶粒，其演化与II型超新星有关。因此，例如在实验室条件下，当 SiC-X 晶粒被摧毁时，会释放出 Xe-S 和 Xe-pr2n 成分的混合物，我们将其命名为 Xe-X。因此，根据我们提出的概念，氙的主要成分除 Xe-S 外，还包括 Xe-P3、Xe-P3n、Xe-pr1n 和 Xe-X，它们分别包含在不同的载相中。对 Murchison CM2 和 Allende CV3 等不同陨石的 NDF 中这些成分丰度的成功计算及其分析表明，上述成分可能是真正的成分。

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引用次数: 0

Gaia Data Release 3: Distribution of Spectral Groups of Near-Earth Asteroids 盖亚数据第 3 版：近地小行星光谱组的分布

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700205

M. Shcherbina, D. A. Kovaleva, B. M. Shustov

引用次数: 0

One-Dimensional Model of Vertical Transport of Chemical Components in the Mars Atmosphere up to the Lower Thermosphere 火星大气层中化学成分垂直迁移至低热层的一维模型

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/s0038094623700041

Y. Kylivnyk, A. S. Petrosyan, A. A. Fedorova, O. I. Korablev

Abstract—

This study is devoted to the analysis of transport of chemical components of the Mars atmosphere. We investigate the turbulent diffusion of chemical components of the Mars atmosphere. To solve this problem in the approximation of diffusion of the minor component, we composed the continuity equation and the corresponding difference scheme. We formulated the boundary conditions in accordance with the available experimental and theoretical data and obtained the required temperature and pressure profiles. For simulation, we chose two models of turbulent diffusion, which were used in subsequent calculations. The simulation was performed using the modified Newton method. The models showed significant differences in the distribution of minor components of the atmosphere, in particular, hydrogen-containing molecules, which indicates the importance of choosing a model for describing turbulent diffusion when constructing a one-dimensional photochemical model of the atmosphere.

摘要--本研究致力于分析火星大气中化学成分的传输。我们研究了火星大气中化学成分的湍流扩散。为了在次要成分扩散近似条件下解决这个问题，我们建立了连续性方程和相应的差分方案。我们根据现有的实验和理论数据制定了边界条件，并获得了所需的温度和压力曲线。为了进行模拟，我们选择了两种湍流扩散模型，并在随后的计算中使用。模拟采用修正牛顿法进行。这两种模型在大气次要成分，特别是含氢分子的分布方面显示出明显的差异，这表明在构建大气一维光化学模型时选择描述湍流扩散的模型非常重要。

引用次数: 0

Manifestations of Anomalous Dissipation in Dusty Plasma in the Solar System: Atmosphereless Cosmic Bodies 太阳系尘埃等离子体的异常耗散表现：无大气层宇宙天体

IF 0.9 4区物理与天体物理 Q3 Physics and Astronomy

Solar System Research

Pub Date : 2024-05-20 DOI: 10.1134/s003809462370003x

S. I. Popel, L. M. Zelenyi

Abstract—

One of the main features that distinguishes dusty plasma from ordinary (not containing charged dust particles) plasma is anomalous dissipation associated with the process of charging dust particles, leading to new physical phenomena, effects and mechanisms. The process of anomalous dissipation is considered in the context of describing the dynamics of dust particles in the dusty plasma of atmosphereless bodies of the Solar System. A description of the oscillations of a dust particle over the surfaces of Mercury, the Moon, and the Martian satellites Phobos and Deimos is presented, the attenuation of which is determined by the charging frequency of the dust particles, which characterizes anomalous dissipation. The possibility of using an approach that takes into account anomalous dissipation to describe plasma-dust processes in the vicinity of comets is discussed. It is shown that anomalous dissipation plays a significant role in determining the possibility of using the model of levitating dust particles in describing dusty plasma over the surfaces of atmosphereless bodies of the Solar System. The results of numerical calculations are presented, confirming the possibility of using this model for a number of atmospherelesso cosmic bodies.

摘要-尘埃等离子体区别于普通（不含带电尘埃粒子）等离子体的主要特征之一是与尘埃粒子带电过程相关的反常耗散，从而导致新的物理现象、效应和机制。反常耗散过程是在描述太阳系无大气层天体尘埃等离子体中尘埃粒子动力学的背景下考虑的。介绍了尘埃粒子在水星、月球、火星卫星火卫一和火卫二表面上的振荡情况，其衰减由尘埃粒子的充电频率决定，这就是反常耗散的特征。讨论了使用一种考虑到反常耗散的方法来描述彗星附近等离子体-尘埃过程的可能性。结果表明，反常耗散在决定是否有可能使用悬浮尘埃粒子模型来描述太阳系无大气层天体表面的尘埃等离子体方面起着重要作用。数值计算的结果证实了对一些无大气层的宇宙天体使用这一模型的可能性。

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