Solar System Research最新文献_第9页

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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700126

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

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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700138

V. D. Borzosekov, N. S. Akhmadullina, A. S. Sokolov, T. E. Gayanova, A. D. Rezaeva, V. D. Stepakhin, E. M. Konchekov, D. V. Malakhov, E. V. Voronova, I. R. Nugaev, V. P. 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. I. Grohovsky, O. N. Shishilov, N. N. Skvortsova

{"title":"Obtaining Plasma–Dust Clouds from Meteoritic Matter, its Analogs and Simulants of Lunar Regolith Using Microwave Discharge","authors":"V. D. Borzosekov, N. S. Akhmadullina, A. S. Sokolov, T. E. Gayanova, A. D. Rezaeva, V. D. Stepakhin, E. M. Konchekov, D. V. Malakhov, E. V. Voronova, I. R. Nugaev, V. P. 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. I. Grohovsky, O. N. Shishilov, N. N. Skvortsova","doi":"10.1134/S0038094624700138","DOIUrl":"10.1134/S0038094624700138","url":null,"abstract":"In the experiment, plasma–dust clouds were obtained from the substance of the Tsarev meteorite, a simulant of lunar regolith LMS-1D and ilmenite concentrate using a microwave discharge in powder media. For each of the samples, the dynamics of the development of the discharge and the formation of a plasma–dust cloud with subsequent relaxation after the end of the microwave pulse were recorded. From the emission spectra of the plasma and the surface of a solid body, the temperatures of the gas, electrons and surface were determined. A comparison of the phase and elemental composition of the initial samples and samples after exposure to plasma showed that there is no significant change in the composition. However, scanning electron microscopy results clearly indicate spheroidization of the original angular and irregularly shaped particles. The appearance of spherical particles is also observed, the dimensions of which are larger than the linear dimensions of the particles in the original sample. The results obtained indicate the possibility of using such experiments to study chemical and plasma-chemical processes of synthesis and modification of substances under conditions of plasma–dust clouds encountered in space phenomena.","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 3","pages":"289 - 314"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1134/S0038094624700138.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141121368","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}

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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700199

T. V. Salnikova, E. I. 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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094623700065

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

{"title":"Potentially Primary Xenon Components in Nanodiamond-Enriched Meteorite Fractions: New Isotopic Compositions and Carrier Phases","authors":"A. V. Fisenko, L. F. Semenova, T. A. Pavlova","doi":"10.1134/S0038094623700065","DOIUrl":"10.1134/S0038094623700065","url":null,"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.","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"240 - 249"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150668","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}

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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700205

M. P. 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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094623700041

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

引用次数: 0

On the Influence of the Rayleigh–Taylor Instability on the Formation of Dust Clouds in the Mesosphere of Mars 论瑞利-泰勒不稳定性对火星中间层尘云形成的影响

IF 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094624700187

Yu. S. Reznichenko, A. Yu. Dubinskii, S. I. Popel

引用次数: 0

The Influence of the Exosphere of an Active Asteroid on the Polarization of Scattered Light and the Possibility of Estimating Its Properties from Ground-Based Measurements 活动小行星外大气层对散射光极化的影响以及通过地基测量估计其特性的可能性

IF 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094623700016

E. V. Petrova

{"title":"The Influence of the Exosphere of an Active Asteroid on the Polarization of Scattered Light and the Possibility of Estimating Its Properties from Ground-Based Measurements","authors":"E. V. Petrova","doi":"10.1134/S0038094623700016","DOIUrl":"10.1134/S0038094623700016","url":null,"abstract":"Celestial bodies which have orbital and physical characteristics typical of asteroids, but episodically exhibit the signs of cometary activity are of particular interest, because the knowledge of the nature of these bodies is necessary to understand the processes of how the Solar System formed and how water was delivered to the terrestrial planets. In the estimation of the properties of an exosphere of an active asteroid (AA) from remote-sensing data, polarimetry can play a prominent role, since the polarization of scattered light is sensitive to the properties of particles in the medium. Numerical simulations of the light scattering by particles in the exosphere around an AA have shown that, depending on the wavelength of the scattered light, the refractive index of particles, and their morphology, the light scattering in the exosphere may both weaken the polarization of light reflected by the surface and enhance it. At the same time, the spectral gradient of polarization may change both towards larger positive values and towards negative ones. At phase angles less than 30°, which are typical of observations of the Main-belt asteroids, the changes in the polarization induced by scattering in the exosphere are small and vary only slightly for particles of different properties. Nevertheless, if the polarizations of light reflected by an asteroid changes relative to the canonical values, this may indicate the presence of the exosphere. At larger phase angles, the influence of scattering in the exosphere on the polarization of an AA is more noticeable, which makes the use of polarimetry promising for studying activity of near-Earth asteroids. This effect should also be taken into account when estimating the albedo of an asteroid by the polarization maximum (according to the Umov law), if a manifestation of activity in this particular asteroid can be expected.","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"196 - 207"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150669","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}

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 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S003809462370003X

S. I. Popel, L. M. Zelenyi

{"title":"Manifestations of Anomalous Dissipation in Dusty Plasma in the Solar System: Atmosphereless Cosmic Bodies","authors":"S. I. Popel, L. M. Zelenyi","doi":"10.1134/S003809462370003X","DOIUrl":"10.1134/S003809462370003X","url":null,"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.","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"220 - 239"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150712","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}

引用次数: 0

Disturbances in the Rotational Dynamics of Asteroid (99942) Apophis at its Approach to the Earth in 2029 小行星（99942）阿波菲斯在 2029 年接近地球时的旋转动力学干扰

IF 0.6 4区物理与天体物理

Solar System Research Pub Date : 2024-05-20 DOI: 10.1134/S0038094623700107

K. S. Lobanova, A. V. Melnikov

{"title":"Disturbances in the Rotational Dynamics of Asteroid (99942) Apophis at its Approach to the Earth in 2029","authors":"K. S. Lobanova, A. V. Melnikov","doi":"10.1134/S0038094623700107","DOIUrl":"10.1134/S0038094623700107","url":null,"abstract":"Using numerical modeling of the rotational dynamics of asteroid (99942) Apophis, the disturbances that occur in the rotational motion of asteroids during their close approaches to the Earth were studied. Such events can lead to significant changes in the speed of the asteroid’s own rotation and the orientation of its rotation axis in space. Assuming that the figure of Apophis is approximated by a triaxial ellipsoid, the dependences of changes in the rotation period of an asteroid on the parameters of the orbit and its rotational state before approaching the Earth were studied. It has been established that the rotation period of Apophis, which is currently about 30 h, may change due to the next approach to Earth in 2029 very significantly—to 10–15 h; in numerical experiments, both acceleration and deceleration of the asteroid’s rotation were observed. Perturbations in the rotational motion of the asteroid noticeably affect its further orbital dynamics as a result of changes in the magnitude of the Yarkovsky effect. It was concluded that as a result of close approach, the average rate of change of the semimajor axis of Apophis’s orbit caused by the Yarkovsky effect, which is currently about 200 m/year, may decrease to 160 m/year or increase to 300 m/year.","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"208 - 219"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150717","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}

引用次数: 0