Solar System Research最新文献

英文中文

Study of the Dynamical Evolution of the Compact Planetary System Kepler-51 开普勒-51紧凑行星系统的动态演化研究

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700394

E. D. Kuznetsov, A. S. Perminov

Abstract—

This paper examines the dynamic evolution of the compact three-planet system Kepler-51. Possible resonant states of the system are analyzed and a search for potential chains of mean motion resonances is carried out. Using the Posidonius software package the dynamic evolution of the system is studied over a time interval of 100 Myr, taking into account tidal interaction. Also, for various initial values of eccentricities, inclinations, arguments of periapsis and longitudes of the ascending nodes of orbits, modeling of the dynamic evolution of the planetary system is carried out within the framework of the semi-analytical theory of motion. It is shown that the compact planetary system Kepler-51 is not resonant. Under initial conditions corresponding to the masses and elements of the planets’ orbits, determined from observations taking into account their errors, the evolution of the system is stable and regular over the studied interval of 100 Myr.

摘要-本文研究了紧凑型三行星系统开普勒-51的动态演化。分析了该系统可能的共振状态，并寻找了平均运动共振的潜在链。利用 Posidonius 软件包研究了该系统在 100 Myr 时间间隔内的动态演化，同时考虑了潮汐相互作用。此外，针对偏心率、倾角、近地点参数和轨道上升节点经度的各种初始值，在半解析运动理论框架内对行星系统的动态演变进行了建模。结果表明，紧凑行星系统开普勒-51 并不共振。在与行星轨道的质量和元素相对应的初始条件下（这些质量和元素是在考虑到其误差的情况下通过观测确定的），该系统的演化在所研究的 100 Myr 间隔内是稳定和有规律的。

引用次数: 0

The Photocenter Shift Phenomenon in Positional Observations of Active Asteroids (6478) Gault and (248370) 2005 QN173/433Р 活动小行星（6478）高尔特和（248370）2005 QN173/433Р定位观测中的光心偏移现象

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700412

S. R. Pavlov, Yu. A. Chernetenko

Abstract

Active asteroids are the Main-Belt asteroids that manifest physical signs of cometary activity, such as the presence of coma and tails and significant changes in brightness. This raises the question of whether these bodies require a more sophisticated approach to specifying the orbital parameters as compared to ordinary asteroids. In this work, we performed a series of improvements in the orbital parameters of active asteroids (6478) Gault and (248370) 2005 QN173/433P both with taking into account nongravitational accelerations (NGAs), which is common for comets, and without this procedure. For time intervals coinciding with the periods of activity of the considered asteroids, we have found statistically significant systematic deviations in the residuals (O–C) between the observed and calculated values in the positional observations of these bodies. Our results show that taking into account the nongravitational acceleration according to the Marsden model does not improve the representation of the observations. We also considered the possibility of the photocenter shift (PS) presence in the positional observations, i.e., the offset between the center-of-light and the center-of-mass. The obtained PS for asteroids (6478) and (248370) are directed away from the Sun with the values of 985 ± 54 and 1145 ± 119 km respectively, which is close to the sizes of the Hill spheres of the bodies. Taking into account the PS effect, one can eliminate the systematic deviations in the residuals for asteroid (248370) and significantly reduce them for asteroid (6478).

摘要活动小行星是主带小行星，它们表现出彗星活动的物理迹象，如出现彗缨和尾巴以及亮度的显著变化。这就提出了一个问题：与普通小行星相比，这些天体是否需要更复杂的方法来指定轨道参数。在这项工作中，我们对活跃小行星(6478)高尔特和(248370)2005 QN173/433P的轨道参数进行了一系列改进，既考虑了彗星常见的非轨道加速度（NGAs），也没有采用这一程序。在与所考虑的小行星的活动期相吻合的时间段内，我们发现这些天体的位置观测数据中观测值与计算值之间的残差（O-C）在统计学上存在显著的系统性偏差。我们的结果表明，根据马斯登模型将非重力加速度考虑在内并不能改善观测结果的代表性。我们还考虑了位置观测中存在光心偏移（PS）的可能性，即光心与质量中心之间的偏移。小行星(6478)和(248370)获得的光心偏移值远离太阳，分别为 985 ± 54 和 1145 ± 119 千米，接近天体希尔球的大小。考虑到 PS 效应，可以消除小行星（248370）残差中的系统偏差，并显著减少小行星（6478）的残差。

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引用次数: 0

Propagation of Hydromagnetic Disturbance Waves and Gravitational Instability in a Magnetized Rotating Heat-Conducting Anisotropic Plasma 磁化旋转导热各向异性等离子体中的水磁扰动波传播和引力不稳定性

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700382

A. V. Kolesnichenko

Abstract—

The hydrodynamic instability of a magnetized, self-gravitating rotating anisotropic plasma is analyzed in the collisionless approximation and considering the heat flux vector based on the modified Chu–Goldberger–Low equations. A dispersion relation is obtained, on the basis of which simplified cases of propagation of low-amplitude disturbance waves and the derivation of modified criteria for hydrodynamic instability are discussed. Using the obtained dispersion relation, three simple cases are treated when the disturbance wave propagates across, along, and obliquely to the magnetic field vector. It is shown that the anisotropy of pressure and heat flow not only changes the classical criterion of the Jeans instability, but also leads to the appearance of new wave modes and causes the appearance of new unstable domains. It has been found that the presence of uniform rotation of the plasma reduces the critical wave number and has a stabilizing effect on the criterion of gravitational instability when the disturbance wave propagates transversely, without having an effect in the case of longitudinal propagation. These results are important for developing evolutionary magnetohydrodynamic models of astrophysical collisionless plasma.

摘要根据修正的 Chu-Goldberger-Low 方程，考虑到热通量矢量，在无碰撞近似条件下分析了磁化自引力旋转各向异性等离子体的流体力学不稳定性。在此基础上，讨论了低振幅扰动波传播的简化情况和流体力学不稳定性修正标准的推导。利用得到的频散关系，处理了扰动波横向、沿磁场矢量和斜向磁场矢量传播的三种简单情况。结果表明，压力流和热流的各向异性不仅改变了杰恩斯不稳定性的经典判据，而且导致了新的波模式的出现，并引起了新的不稳定域的出现。研究发现，当扰动波横向传播时，等离子体的均匀旋转会降低临界波数，并对引力不稳定性准则产生稳定作用，而在纵向传播的情况下则不会产生影响。这些结果对于开发天体物理无碰撞等离子体的进化磁流体动力学模型非常重要。

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引用次数: 0

Impact Craters on Earth with a Diameter of More than 200 km: Numerical Modeling 直径超过 200 千米的地球撞击坑：数值建模

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700370

B. A. Ivanov

Abstract

The three largest impact craters, the remains of which have been found on Earth to date, had diameters of about 200 km immediately after formation. The search for traces of larger impact structures continues. This paper presents the results of numerical modeling of the formation of terrestrial impact craters larger than those already found. It is shown that the inferred geothermal gradient significantly influences the initial geometry of the impact melt region, which may facilitate the search for the remains of deeply eroded ancient impact structures.

摘要迄今为止在地球上发现的三个最大的撞击坑遗迹，形成后的直径约为 200 公里。寻找更大的撞击结构痕迹的工作仍在继续。本文介绍了对比已发现的撞击坑更大的陆地撞击坑的形成过程进行数值模拟的结果。结果表明，推断的地热梯度对撞击熔化区的初始几何形状有很大影响，这可能有助于寻找深度侵蚀的古代撞击结构的遗迹。

引用次数: 0

On the Nature of Electrophone Phenomena Accompanying the Passage of Meteoric Bodies through the Earth’s Atmosphere 论流星体穿过地球大气层时伴随的电声现象的性质

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700424

A. D. Filonenko

Abstract—

The paper briefly discusses hypotheses about the nature of a centuries-old mysterious phenomenon, for which there is still no clear explanation. Its essence is that an observer, usually located at a distance of 50–100 km from a flying meteor body, sometimes hears sound simultaneously with its radiation. It seems that sound travels at the speed of light. Historically, the situation was such that it was only no more than sixty years ago that attempts to instrumentally study this unusual phenomenon began. The difficulty of these searches is also due to the fact that only a few percent of the total number of observed meteoroids have this property. About forty years ago it was discovered that meteoroids can emit electromagnetic pulses of varying duration and frequency composition. However, it turned out that this fact does not always have an unambiguous relationship to electrophonic phenomena. This paper provides a brief overview of the most meaningful hypotheses and experiments of past years. It is possible that this phenomenon is of a fundamental nature and its study can introduce previously unknown information into science.

摘要--本文简要讨论了关于一种神秘现象性质的假设，这种现象已有数百年的历史，至今仍没有明确的解释。其本质是，通常位于距离飞行流星体 50-100 公里处的观察者，有时会听到与流星体辐射同时出现的声音。声音似乎是以光速传播的。从历史上看，这种情况直到六十多年前才开始尝试用仪器研究这种不寻常的现象。这些研究之所以困难，还因为在观测到的流星体总数中，只有百分之几具有这种特性。大约四十年前，人们发现流星体可以发射持续时间和频率成分各不相同的电磁脉冲。然而，事实证明，这一事实并不总是与电声现象有着明确的关系。本文简要概述了过去几年中最有意义的假设和实验。这种现象有可能具有基本性质，对它的研究可以为科学引入以前未知的信息。

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引用次数: 0

Determining Optimal Parameters for Mercury’s Magnetospheric Current Systems from MESSENGER Observations 通过 MESSENGER 观测确定水星磁层电流系统的最佳参数

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700400

A. S. Lavrukhin, I. I. Alexeev, D. V. Nevsky

Abstract

We use a paraboloid model of Mercury’s magnetosphere and magnetometer data from the MESSEN-GER spacecraft obtained in April 2011 to determine the optimal parameters of Mercury’s magnetospheric current systems, in the sense that they yield the smallest discrepancy (less than 10 nT) between model predictions and measurements. The obtained model data are compared with experimental data and the KT17 model of Mercury’s magnetospheric magnetic field.

摘要我们利用水星磁层抛物面模型和 2011 年 4 月从 MESSEN-GER 航天器获得的磁强计数据，确定了水星磁层电流系统的最佳参数，即模型预测值与测量值之间的差异最小（小于 10 nT）。获得的模型数据与实验数据和水星磁层磁场 KT17 模型进行了比较。

引用次数: 0

Astrometry and Photometry of Potentially Dangerous Asteroid 65690 (1991 DG) 潜在危险小行星 65690（1991 DG）的天体测量和光度测量

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700369

A. V. Devyatkin, D. L. Gorshanov, V. N. Lvov, S. D. Tsekmeister, S. N. Petrova, A. A. Martyusheva, K. N. Naumov

Abstract—

In 2020, two telescopes of the State Astrophysical Observatory of the Russian Academy of Sciences, ZA-320M and MTM-500M, obtained series of observations of the potentially dangerous asteroid 65690 (1991 DG) during its approach to the Earth and carried out their astrometric and photometric processing. Using the coordinates of the asteroid and observations from the MRS site, the orbit of the asteroid was clarified, and the circumstances of the approaches to the Earth and Mars were determined, and an assessment was made of the influence of nongravitational effects on its orbit. Based on the results of photometric processing of the asteroid, a light curve was constructed and the period of its axial rotation was determined: P = 4.3193 ± 0.0028 h.

摘要--2020 年，俄罗斯科学院国家天体物理观测台的两台望远镜 ZA-320M 和 MTM-500M 在有潜在危险的小行星 65690（1991 年 DG）接近地球期间对其进行了系列观测，并对其进行了天体测量和光度处理。利用小行星的坐标和来自 MRS 站点的观测数据，明确了小行星的轨道，确定了接近地球和火星的情况，并评估了非轨道效应对其轨道的影响。根据对该小行星的光度处理结果，构建了一条光曲线，并确定了其轴向旋转周期：P = 4.3193 ± 0.0028 h。

引用次数: 0

Analysis of Water in the Regolith of the Moon Using the LASMA-LR Instrument During the Luna-27 Mission 在月球-27 飞行任务期间利用 LASMA-LR 仪器分析月球岩石中的水分

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700436

A. E. Chumikov, V. S. Cheptsov, T. A. Abrahamyan

Abstract—

Determining water concentrations in the polar regions of the Moon is one of the priority tasks of a number of space missions and, in particular, the Luna-27 mission. The complex of scientific equipment of the Luna-27 spacecraft includes time-of-flight laser ionization mass spectrometer LASMA-LR, the main task of which is to analyze the elemental composition of the regolith at the landing site. The design and configuration of the flight instrument is adapted for the analysis of regolith and was not originally intended for the study of volatile compounds. However, due to the importance of determining the water content in regolith, we reviewed some approaches to analyzing samples during lunar missions and assessed the applicability of LASMA-LR and the laser ionization mass spectrometry method in general for identifying water in regolith. It has been established that using this instrument it is possible to detect water in regolith, including determining its state (chemically bound and unbound water). Moreover, the conditions for sampling the regolith and delivering it to the soil receiving device of the instrument are critically important for the analysis, since under the conditions of the lunar surface, sublimation of ice is possible before the samples are analyzed. This technique has advantages over some other methods of analyzing water and/or ice used in space experiments, and can be used in the study of a number of planets and bodies of the Solar System.

摘要-确定月球极地地区的水浓度是一些空间飞行任务，特别是月球-27 飞行任务的优先任务之一。月球-27 号航天器的综合科学设备包括飞行时间激光电离质谱仪 LASMA-LR，其主要任务是分析着陆点的残积岩的元素组成。该飞行仪器的设计和配置适合于分析沉积物，最初并不是用于研究挥发性化合物。但是，由于确定岩石中水含量的重要性，我们审查了在月球飞行任务期间分析样品的一些方法，并评估了 LASMA-LR 和激光电离质谱法在确定岩石中水含量方面的适用性。已经确定，使用该仪器可以探测到岩石中的水，包括确定其状态（化学结合水和非结合水）。此外，对岩石取样并将其送入仪器的土壤接收装置的条件对分析至关重要，因为在月球表面的条件下，在对样品进行分析之前，冰有可能升华。与空间实验中使用的其他一些分析水和（或）冰的方法相比，这种技术具有优势，可用于研究太阳系的一些行星和天体。

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引用次数: 0

Research Progress in High-Energy Electron Flux Prediction Methods in Geosynchronous Orbit 地球同步轨道高能电子通量预测方法的研究进展

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-09-09 DOI: 10.1134/s0038094624700357

Ke Han, Ying Chu, Jie Wan, Cheng-gang Jin, De-quan Zheng, Peng E

Abstract

The increase in energetic electron flux is a complex nonlinear phenomenon with a profound impact on satellite operations in geosynchronous orbit. Previous research, conducted both locally and internationally, has developed models relying on extensive data to predict occurrences associated with the amplification of high-energy electron fluxes. This study conducts a comprehensive examination of significant research discoveries in the field, with a specific focus on selecting prediction factors and methods for designing forecast models. The study introduces key features of solar wind parameters and their correlation with high-energy electron fluxes, emphasizing the selection of forecast factors. Additionally, it highlights the attributes of geomagnetic indices and their relationship with solar wind parameters. Linear and nonlinear models are presented, with linear models categorized as single-input and multi-input, and nonlinear models classified as single-model design and fusion-model design. The study also explores shallow and deep models as distinct methodologies in nonlinear modeling. In conclusion, this study provides an overview of current research findings and approaches while offering insights into the future development patterns in this domain for the forthcoming term.

摘要高能电子通量的增加是一种复杂的非线性现象，对地球同步轨道上的卫星运行有着深远的影响。国内外以前开展的研究已经建立了一些模型，这些模型依靠大量数据来预测与高能电子通量放大有关的现象。本研究对该领域的重要研究发现进行了全面审查，特别侧重于选择预测因子和设计预测模型的方法。研究介绍了太阳风参数的主要特征及其与高能电子通量的相关性，强调了预测因子的选择。此外，研究还强调了地磁指数的属性及其与太阳风参数的关系。介绍了线性和非线性模型，线性模型分为单输入和多输入，非线性模型分为单模型设计和融合模型设计。研究还探讨了非线性建模中作为不同方法的浅层模型和深层模型。总之，本研究概述了当前的研究成果和方法，同时对该领域未来的发展模式提出了见解。

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引用次数: 0

Age Estimation of Young Asteroid Pairs 年轻小行星对的年龄估计

IF 0.9 4区物理与天体物理 Q4 ASTRONOMY & ASTROPHYSICS

Solar System Research

Pub Date : 2024-08-01 DOI: 10.1134/s0038094624700473

V. S. Safronova, E. D. Kuznetsov

Abstract—

In order to estimate the age, the work examined the probabilistic evolution of three young pairs of asteroids in close orbits: (87 887) 2000 SS286—(415 992) 2002 AT49, (320 025) 2007 DT76—(489 464) 2007 DP16, (21 436) Chaoyichi—(334 916) 2003 YK39. In the numerical simulation, along with gravitational disturbances, the Yarkovsky effect in the form of a secular drift of the orbital semimajor axis was taken into account. For each pair of asteroids, 25 evolution scenarios were considered, corresponding to different combinations of obliquities of the asteroids’ rotation axes and, correspondingly, different drift rates of the semimajor axes due to the Yarkovsky effect. For each asteroid, 1000 clones were generated. Age estimates were obtained based on analysis of moment distributions: (1) low relative-velocity close encounters of asteroids of pair to distances on the order of the Hill sphere at a relative speed of several units of the escape velocity and (2) achievement of minimum values of the Kholshevnikov metric, which characterizes the distance between orbits. The following age estimates for young asteroid pairs were obtained: (87 887) 2000 SS286 and (415 992) 2002 AT49 from 7.58 ± 0.04 to 8.80 ± 0.04 kyr; (320 025) 2007 DT76 and (489464) 2007 DP16 from 15.5 ± 1.0 to 58.6 ± 16.0 kyr; (21 436) Chaoyichi and (334 916) 2003 YK39 from 32.3 ± 0.1 to 102.6 ± 0.7 kyr.

摘要为了估算年龄，这项工作研究了三对年轻的近轨道小行星的概率演变：(87 887) 2000 SS286-(415 992) 2002 AT49、(320 025) 2007 DT76-(489 464) 2007 DP16、(21 436) Chaoyichi-(334 916) 2003 YK39。在数值模拟中，除了引力扰动外，还考虑了以轨道半长轴周期漂移形式出现的雅尔科夫斯基效应。针对每对小行星，考虑了 25 种演化情况，对应于小行星旋转轴的不同斜度组合，以及相应的雅尔科夫斯基效应导致的不同半主轴漂移率。每颗小行星生成 1000 个克隆。年龄估计是根据对矩分布的分析得出的：(1)一对小行星以希尔球数量级的低相对速度近距离相遇，相对速度为逃逸速度的几个单位；(2)达到霍尔舍夫尼科夫度量的最小值，该度量表征了轨道之间的距离。年轻小行星对的年龄估计如下：(87 887) 2000 SS286 和 (415 992) 2002 AT49 从 7.58 ± 0.04 千年到 8.80 ± 0.04 千年；(320 025) 2007 DT76 和 (489464) 2007 DP16 从 15.5 ± 1.0 千年到 58.6 ± 16.0 千年；(21 436) Chaoyichi 和 (334 916) 2003 YK39 从 32.3 ± 0.1 千年到 102.6 ± 0.7 千年。

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