Solar System Research最新文献

{"title":"Non-Hydrostatic Stresses in the Martian Interior without Accounting for the Long-Wavelength Component","authors":"A. V. Batov,&nbsp;T. V. Gudkova","doi":"10.1134/S0038094625600295","DOIUrl":"10.1134/S0038094625600295","url":null,"abstract":"<p>The calculation of nonhydrostatic stresses in the interior of Mars is carried out without taking into account the long-wave component. The numerical solution of the system of equations of elastic equilibrium for a gravitating planet was carried out on a grid with a resolution of 1° × 1° in latitude and longitude. Data on the topography and gravitational field of the planet, starting with the seventh harmonic, were used as boundary conditions. Most of the epicenters of marsquakes are located in zones of extensions and sufficiently large tangential stresses arising as a result of the planet’s deviation from the state of hydrostatic equilibrium. The directions of the main stress axes and their correspondence to the strike of geological structures on the planet’s surface are given.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145168841","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}

{"title":"Turbulent Micropolar Fluid as a Continuous Medium with an Internal Vortex Structure","authors":"A. V. Kolesnichenko","doi":"10.1134/S0038094625600453","DOIUrl":"10.1134/S0038094625600453","url":null,"abstract":"<p>A modern approach to thermodynamic modeling of developed turbulent flows of micropolar compressible fluid is considered, based on the application of the formalism of extended irreversible thermodynamics. The description of turbulent motion of turbulent fluid is carried out within the framework of the generalized continuum model consisting of two interconnected open subsystems—the averaged motion subsystem and the turbulent chaos subsystem (associated with small-scale vortex motion of the fluid). This made it possible to construct an evolutionary hyperbolic second-order closure model based on nonlinear constitutive equations of turbulent flow transfer using the generalized Gibbs equation and the general form of the entropy flux. The proposed methodology is in good agreement with the idea of A.N. Kolmogorov on the possibility of representing the pseudovector of angular velocity as an internal parameter for a thermodynamically open turbulent system if the scale of the differential grid exceeds the size of the mesovortices. It is this consideration that made it possible to develop continuous equations of turbulence that reflect the effect of internal rotation of turbulent mesovortices, as well as the case of a turbulent fluid with anisotropy of a vortex nature, which is related to the nonzero antisymmetric part of the Reynolds tensor. The results obtained can be used in studying the turbulent motions of micropolar fluids in the depths of stars, giant planets, as well as in the atmosphere of the Sun and other cosmic bodies.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145169325","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}

{"title":"Electromagnetic Phenomena Induced by Charged Dust Particles Dynamics in Planetary Atmospheres: Laboratory Simulations and Field Observations","authors":"Mohamad E. Abdelaal,&nbsp;Alexander V. Zakharov","doi":"10.1134/S0038094625600519","DOIUrl":"10.1134/S0038094625600519","url":null,"abstract":"<p>Dust electrification and its associated electromagnetic (EM) emissions play a critical role in atmospheric and near-surface dynamics across planetary environments. This study provides a synthesis of recent work under publication that investigates the mechanisms of charge accumulation, electrostatic discharge, and electromagnetic radiation generation in dust-laden flows under both terrestrial and Mars-analog conditions, using a combined approach of analytical modeling, laboratory experiments, and field measurements. Laboratory experiments were conducted in the Earth conditions and in low-pressure CO₂-rich environments to simulate Martian conditions, employing silicate and basaltic samples across a range of grain sizes. The results demonstrate that triboelectric and tunneling charge transfer mechanisms, activated during vortex-driven particle dynamics, can induce transient discharges that generate broadband electromagnetic signals in the ~120–1500 kHz range. Under simulated Martian conditions, Paschen breakdown behavior was experimentally verified, confirming significantly lower breakdown thresholds compared to Earth’s atmosphere. Complementary field measurements carried out in the Kalmykian desert (Russia) further revealed that low humidity and intense solar radiation, even in the presence of moderate wind speeds, enhance dust electrification and discharge activity, leading to detectable EM emissions. Data were recorded using the Electromagnetic Analyzer (EMA), originally developed for Mars surface studies. Analysis of the recorded EM signal using time-domain analysis, Fast Fourier Transform (FFT), and continuous wavelet transform (CWT) revealed distinct amplitude-frequency signatures that correlate with particle properties and environmental drivers. These findings establish a new conceptual framework for understanding dust-driven EM phenomena in planetary atmospheres and underscore the applied relevance of electromagnetic diagnostics for future Mars, Moon, and Venus missions.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145168840","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}

{"title":"Photochemical Equilibrium and Ozone Balance Equation in the Nighttime Hydroxyl Layer on Mars","authors":"D. S. Shaposhnikov,&nbsp;A. V. Rodin","doi":"10.1134/S0038094625600337","DOIUrl":"10.1134/S0038094625600337","url":null,"abstract":"<p>Combined measurements of ozone (O₃₎ and vibrationally excited hydroxyl (OH*) emissions allow determination of atomic oxygen (O) and hydrogen (H) concentrations, which are otherwise difficult to measure directly. This method is applicable only when ozone photochemical equilibrium (OPE) conditions are met. This paper is the first to investigate OPE in the nighttime atmosphere of Mars and its relationship to OH* emissions. Based on numerical modeling using data from Mars Climate Database (MCD), the spatiotemporal distributions of ozone deviations from the equilibrium state and the ratio of ozone lifetimes at current and equilibrium concentrations are analyzed. Two main OPE criteria are derived. The results show that OPE is satisfied over wide regions (65–90 km) in the second half of the Martian year (<i>L</i>_s = 180°–360°), especially at polar and midlatitudes. However, the regions with observed OH* concentrations ([OH*] <span>( geqslant )</span>100 cm^–3) and satisfied OPE criteria are limited to the first half of the year (<i>L</i>_s = 0°–180°) and altitudes of 50–70 km. This indicates the difficulty of applying the method for retrieving O and H concentrations from OH* under Martian conditions without additional adaptation of the equilibrium criteria. Therefore, we test a criterion derived from the basic principles of photochemistry of the terrestrial mesosphere, mesopause, and lower thermosphere. The study highlights the need for further observations and refined models to correctly interpret chemical processes in the Martian atmosphere.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145168220","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}

{"title":"Spectra of Earth-like Exoplanets with Different Rotation Periods","authors":"S. I. Ipatov,&nbsp;J. Y-K. Cho","doi":"10.1134/S0038094625600234","DOIUrl":"10.1134/S0038094625600234","url":null,"abstract":"<p>At present, planets like the Earth have been found near other stars. We investigate the spectra of Earth-like planets but with different axial rotation periods. Using the general circulation model of the atmosphere called the Community Climate Model (CCM3) and considering the atmospheric circulation lasting for two years, we calculated the radiation spectra of the Earth and the exo-Earth rotating with periods of 1 and 100 days, respectively. The radiation spectra of the atmospheres were calculated with the SBDART code. We analyzed the spectrum of upward radiation at altitudes of 1 and 11 km in wavelength ranges of 1 to 18 μm and 0.3 to 1 μm. The following common features were obtained for the Earth and the exo-Earth: (1) the planets exhibit a wide absorption band of CO₂ around 14 μm; (2) the radiation spectra at different locations near the equator show no significant differences (however, for some regions, e.g., near the poles, there can be considerable differences in the spectra); and (3) if the spectrum is integrated over the entire disk of the Earth/exo-Earth, the difference in the spectral signal obtained in observations from different directions becomes substantially lower than the difference between the results of observations of individual regions of the planets; however, the difference in the integrated signal of the spectrum for the Earth and the exo-Earth is noticeable (for example, this difference is noticeable for the spectrum obtained at an altitude of 11 km, when observing the South and North Poles; though, the difference is small, if one observes the whole disk from different equatorial directions). The differences in the spectra of exoplanets, which differ from the Earth only in axial rotation period, are comparable to the differences associated with changes in the angle of viewing the planet. Consequently, if the observation angle is not known, the analysis of the spectrum of the planet cannot be used to determine its axial rotation period. The maximal differences in the spectra of Earth-like exoplanets were obtained for wavelengths of about 5–10 and 13–16 μm. By analyzing the spectrum at wavelengths around 9.4–10 µm, we can determine whether the atmosphere of the exoplanet contains ozone or not. In the diagrams for the upward radiation at an altitude of 11 km, there is no local minimum at wavelengths of 9.4–10 µm if ozone is absent; and, when the models contain ozone, this minimum is present. Since ozone is essential for life, the 9.4–10 µm band may be important for future observations of Earth-like exoplanets.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144990390","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}

{"title":"Geological Structure of the Upper Part of Nirgal Vallis, Mars","authors":"E. S. Cholovskaia,&nbsp;M. A. Ivanov","doi":"10.1134/S0038094625600374","DOIUrl":"10.1134/S0038094625600374","url":null,"abstract":"<p>Photogeological analysis of the upper Nirgal Vallis area, located in the northwestern part of the Noachis Terra highland plain, has shown that there were at least two episodes of fluvial activity in this area: the Noachis, which resulted in the formation of channels on the slopes of the ancient volcano, and the Hesperian, which formed Her Desher and Nirgal Vallis and channels on the southern slope of the northwestern ancient uplift. Similar results for determining the absolute model age of the formation of channels and large craters may indicate that impact activity in this region was the main cause of episodic warming. In addition, glacial activity may have occurred in the study area during early Amazonian times, forming an erosion area near Her Desher Vallis.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144990331","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}

{"title":"Resonant Interactions of Poincaré Waves in the Shallow Water Approximation","authors":"D. A. Klimachkov,&nbsp;A. S. Petrosyan","doi":"10.1134/S0038094625600350","DOIUrl":"10.1134/S0038094625600350","url":null,"abstract":"<p>The paper develops a weakly nonlinear theory of Poincaré waves. The nondegeneracy of the Poincaré wave dispersion law leads to the presence of resonant interactions in perturbation theory. A study of the dispersion relation of Poincaré waves showed that three-wave interactions are absent in the quadratic nonlinear approximation. In this paper, a linear equation of the envelope is derived. A qualitative study of the dispersion law showed the existence of four-wave interactions of Poincaré waves. Equations of nonlinear interactions of four waves for the amplitudes of Poincaré waves are derived. The Manley–Rowe equations are obtained, which determine the distribution of energy and its transfer between interacting waves. The nonlinear dynamics of interacting waves is investigated. The saturation effect of Poincaré waves, which is important for geophysical hydrodynamics, has been predicted. An analytical solution is obtained that describes the saturation effect of Poincaré waves in time.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1134/S0038094625600350.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144990526","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}

{"title":"Models of the Night-Sky Brightness and the Efficiency of Searching for Exoplanets with the Microlensing Method","authors":"S. I. Ipatov","doi":"10.1134/S003809462560026X","DOIUrl":"10.1134/S003809462560026X","url":null,"abstract":"<p>We analyze photometric observations of stars, which experienced microlensing events at the considered time, in order to compare the efficiency of detecting exoplanets in observations performed at thirteen different telescopes and with several approaches to the selection of observable events. In constructing an algorithm of the optimal selection of targets for these observations and in comparing the detection efficiencies for several telescopes, we considered models of the night-sky brightness that satisfy the data of infrared observations carried out in 2011 with the Optical Gravitational Lensing Experiment (OGLE) telescope and the RoboNet telescopes (FTS, FTN, and LT) used to search for planets with the microlensing method. The considered models of the night-sky brightness can be used for various observations (not only microlensing events). The time intervals, during which microlensing events can be observed, were determined with accounting for the positions of the Sun and the Moon and the other constraints on the telescope pointing. Our algorithm allows us to determine the already known microlensing events that are accessible for observation with a particular telescope and to select targets, for which the probability of detecting an exoplanet is maximal. The events, which would maximize the probability of detecting exoplanets, were selected for observations. The probability of detecting an exoplanet is usually proportional to the mirror diameter of a telescope. Telescopes with a wider field of view, such as the OGLE, are more effective in finding new microlensing events. To observe different microlensing events, it is usually better to use different nearby telescopes. However, all such telescopes are often better to use for observing the same event in those relatively short time intervals that correspond to the peak brightness of the event.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144990530","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}

{"title":"Constructing an Initial Confidence Region Far from the Observational ARC and Estimating the Probability of an Asteroid Impact with the Earth","authors":"A. P. Baturin","doi":"10.1134/S0038094625600246","DOIUrl":"10.1134/S0038094625600246","url":null,"abstract":"<p>A method for reducing nonlinearity in the problem of asteroid orbit determination is considered. The method is based on the use of variables that take into account the stretching of the initial confidence region mainly along the trajectory when the initial epoch is located far from the observational arc. It is shown that in this case, the nonlinearity of the inverse problem is revealed only along the largest axis of the confidence ellipsoid, which is directed almost along the trajectory of the object, while the other axes are not deformed. This allows us to introduce new variables in which one (largest) axis is curved and approximated using polynomials, while the remaining axes remain the same as in the confidence ellipsoid. The confidence region in the new variables is an ellipsoid, which makes it possible to fill it with a cloud of random points according to the law of multidimensional normal distribution and, thus, significantly increase their number. In addition, it is shown that with a significant distance of the initial epoch from the observational arc, the coordinates and velocities noticeably correlate, which simplifies the approximation of the point cloud using an ellipsoid. The method was used to estimate the probability of a collision with the Earth (and the Moon) of potentially dangerous asteroids 2024 YR4, 2023 DO and 2018 CB in their upcoming closest approach.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144918354","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}

{"title":"Precise Orbit Determination for Cislunar Space Targets Based on Ground/Space/Lunar Based Integrated Optical Observation Model","authors":"Zhenqi Wang,&nbsp;Zhongmiao Sun,&nbsp;Bin Guan,&nbsp;Jianguo Yan,&nbsp;Shangbiao Sun,&nbsp;Wanling Yang,&nbsp;Jean-Pierre Barriot","doi":"10.1134/S0038094625600313","DOIUrl":"10.1134/S0038094625600313","url":null,"abstract":"<p>Cislunar space, as a strategically significant domain for humanity’s future survival and development, has become a new battleground for deep space exploration activities among leading spacefaring nations. Driven by the growing demands for deep space exploration missions, the monitoring and early warning of cislunar space debris have increasingly become a priority. Precise orbit determination (POD) of cislunar space targets provides essential support for debris surveillance. Against this backdrop, this study proposes a ground/space/lunar integrated optical observation model, implemented through SPOT (Small Body and Planets Precise Orbit Determination Toolkit)—a software platform independently developed by Wuhan University’s Planetary Geodesy Team. We conducted numerical simulations for POD of targets at Earth–Moon libration points L1, L4, and L5. The results demonstrate that the orbit determination accuracy using only ground-based observations is on the order of several hundred meters. Space-based observations can serve as a valuable supplement to ground-based data, providing a modest improvement in accuracy. However, the addition of lunar-based observations significantly enhances the orbit determination accuracy, reducing position errors and uncertainties to the order of tens of meters. Furthermore, variations in the noise level of lunar-based observations have a stronger impact on orbit determination accuracy than space-based observations. Finally, comparative experiments verify the necessity of solving the solar radiation pressure coefficient Cr for improving orbit determination accuracy. These findings highlight the tremendous potential of lunar-based optical observations in achieving high-precision orbit determination for cislunar space targets and provide valuable insights for future advancements in deep-space situational awareness and autonomous navigation.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144918355","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}