Solar System Research最新文献

{"title":"Spatial and Genetic Relationships of Volcanic Coronae and Large Volcanoes of Venus","authors":"E. N. Guseva,&nbsp;M. A. Ivanov","doi":"10.1134/S0038094624601890","DOIUrl":"10.1134/S0038094624601890","url":null,"abstract":"<p>We analyzed regions with concentrations of coronae that are sources of young lava fields and large volcanoes on Venus and established the following: (1) such coronae and volcanoes represent genetically unrelated structures that are spatially separated in many regions of the planet, while in some regions they occur together or only coronae or only volcanoes are present; (2) coronae that are sources of lava fields are associated with regional zones of extension—belts of grooves and/or rift zones—whereas volcanoes show a weaker association with these zones; (3) dome-shaped coronae are concentrated on the surface of Venus in zones of rift fracturing, primarily in the Ulfrun and Parga regions. This association of volcanic coronae with rifts is likely explained by the reactivation of coronae during the late Atlian period of the planet’s geological history; (4) large volcanoes are more widely distributed across the surface of Venus than dome-shaped coronae. Approximately half of the volcanoes are concentrated in the Ulfrun, Parga, and Eistla regions. Their localization is not linked to regional zones of extension; (5) the identified regions of concentration of large volcanoes and dome-shaped coronae, which are sources of lava fields, mark the areas of young volcanic activity on Venus (Ulfrun, Parga, and Eistla).</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":"https://link.springer.com/content/pdf/10.1134/S0038094624601890.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144918356","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":"Low-Energy Transit Trajectories Near Libration Points","authors":"A. V. Ivanyukhin","doi":"10.1134/S0038094625600076","DOIUrl":"10.1134/S0038094625600076","url":null,"abstract":"<p>To increase the efficiency of interplanetary flights, it is advisable to use low-energy trajectories with a small change energy on transfer between massive bodies. The paper considers an approach to designing transit trajectories based on the flyby of libration points L1 and L2 with near-zero velocity, which corresponds to the minimum possible energy change on the trajectory. In the model of a circular restricted three-body problem, these trajectories correspond to motion over invariant manifolds of libration points. Transit trajectories are modeled, and their parameters (capture duration and orbital parameters) are estimated within the framework of the circular and elliptical three-body problem. The influence of the ratio of the masses of massive bodies and the eccentricity of the orbit of a smaller body on the parameters of low-energy transit trajectories in a elliptic restricted three-body problem is analyzed. Examples of trajectories suitable for practical use in interplanetary missions, in the Earth–Moon system, in the Jupiter and Saturn systems are considered.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161467","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":"Daylight Visibility of Jupiter with the Naked Eye","authors":"Ki-Won Lee,&nbsp;Byeong-Hee Mihn,&nbsp;Sang Hyuk Kim,&nbsp;Young Sook Ahn","doi":"10.1134/S003809462560009X","DOIUrl":"10.1134/S003809462560009X","url":null,"abstract":"<p>This study examines Korean historical records of daylight sightings of Jupiter to estimate the empirical limiting magnitude for observing celestial bodies without optical aid during daylight. Using sources such as <i>Joseonwangjo-Sillok</i> (The Veritable Records of the Joseon Dynasty), <i>Seungjeongwon-Ilgi</i> (The Daily Records of the Royal Secretariat of the Joseon Dynasty), and <i>Donggung-Ilgi</i> (The Daily Records of the Royal Education Bureau for the Crown Prince of the Joseon Dynasty), we identified 40 instances of daylight observations of Jupiter during the Joseon dynasty (1392–1910). Employing astronomical algorithms and modern ephemeris, we calculated sunrise, solar transit, and sunset times to identify the observation hour, confirming whether the events occurred during daytime or twilight. Additionally, we determined the azimuth and magnitude of Jupiter during each recorded event to verify the direction and brightness of the observed phenomenon. Our analysis yielded the following key findings: (1) The records of daylight sightings of Jupiter are concentrated in the 16th and 17th centuries, corresponding to prolonged periods of solar activity minima. (2) These observations occurred during broad daylight rather than twilight. (3) The limiting magnitude for unaided daylight observations of a celestial body is at least –2.1.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161482","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":"Assessment of the Impact of Meteor Explosions on the Surface of Venus","authors":"V. V. Shuvalov,&nbsp;B. A. Ivanov","doi":"10.1134/S0038094625600180","DOIUrl":"10.1134/S0038094625600180","url":null,"abstract":"<p>In addition to craters, the surface of Venus contains radiatively bright and dark patches, the formation of which is believed to be caused by the impact of a shock wave. Estimates based on approximate models of asteroid deceleration in the atmosphere and point explosions substantiate the assumption that dark spots arise as a result of strong destruction (vaporization) of stones by a shock wave near the epicenter of the explosion at pressures of about 1–10 GPa, and the light outer part of the splotches is explained by the blowing away of small particles by an air flow at velocities of about 100 m/s at greater distances. Direct calculations of the fragmentation and braking of asteroids with sizes of 0.6–1 km carried out in this work showed that the maximum pressure values are significantly lower than those required to destroy the rocks, and it is concluded that a more probable mechanism for the formation of dark spots is the melting of the surface layer by thermal radiation from the bolide.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 7","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161888","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":"Organic Matter in Titan: Models of Internal Structure","authors":"A. N. Dunaeva,&nbsp;V. A. Kronrod,&nbsp;O. L. Kuskov","doi":"10.1134/S0038094625600088","DOIUrl":"10.1134/S0038094625600088","url":null,"abstract":"<p>Titan, Saturn’s largest moon, is unique in its composition, structure, and formation history. Titan stands out among other bodies in the Solar System due to its dense nitrogen-methane atmosphere with a variety of organic compounds and a surface covered with liquid hydrocarbons. Based on cosmochemical and geophysical data, equations of state of meteoritic matter and H₂O (water, water ice) models of the internal structure of Titan, composed of carbonaceous (CI/CM) and ordinary (L/LL) chondrites, with different contents of organic material (OM) of low (ρ_OM ~ 1.3−1.4 g/cm³) and high (1.4 &lt; ρ_OM &lt; 2.2 g/cm³) density have been constructed. In the absence of OM, three-layer models of a partially differentiated satellite with an outer water-ice shell, an intermediate rock-ice mantle, and an inner CI/CM or L/LL core may be implemented. The presence of an impurity OM with a density 1.3–1.8 g/cm³ in Titan’s chondrite material provides the possibility of transition from three-layer partially differentiated models of the satellite to two-layer models of full differentiation (without rock-ice mantle)—structures free from restrictions on the melting of mantle ice. The structure of a fully differentiated Titan generally includes: a water-ice shell with a mandatory internal ocean and a layer of partially melted high-pressure V-VI ices and a central CI/CM or L/LL chondrite core with a radius of ~2100 km. Such models without OM admixture do not satisfy the conditions of conservation of mass and moment of inertia of the satellite; their consistency with geophysical constraints is due to the presence of OM in amounts of 10−22 wt % and 20−28 wt % in the CI/CM and L/LL cores, respectively. Models of Titan with high density OM (ρ_OM &gt; 1.8 g/cm³) do not suggest separation of the ice and rock components, the satellite remaining partially differentiated. The estimates of the organic material content of Titan are consistent with those for a number of other icy moons of the giant planets and most Kuiper belt objects that formed beyond the snow line. This may indicate a common reservoir of precursor material in the outer Solar System and also suggests a potential genetic link between celestial bodies in this region, which requires further study.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 6","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-07-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145171295","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 Noise in the Near-Surface Martian Atmosphere: Research Methods","authors":"M. E. Abdelaal,&nbsp;I. V. Dokuchaev,&nbsp;I. A. Kuznetsov,&nbsp;I. A. Shashkova,&nbsp;A. N. Lyash,&nbsp;A. E. Dubov,&nbsp;Y. A. Obod,&nbsp;A. A. Kartasheva,&nbsp;G. G. Dolnikov,&nbsp;A. V. Zakharov","doi":"10.1134/S0038094625600143","DOIUrl":"10.1134/S0038094625600143","url":null,"abstract":"<p>The paper considers the phenomenon of electromagnetic (EM) noise during the dynamics of dust particles in a fairly dense plasma-dust environment. The study combines theoretical and experimental concepts of dust charging mechanisms, observation methods, including laboratory modeling, and measurements of noise signals in terrestrial arid regions. A key objective is to characterize the frequency spectra of electromagnetic radiation generated during these processes, particularly in the low and medium frequency ranges (kHz to MHz), which are relevant for understanding dust storms and their role in Mars’ atmospheric electricity. The findings provide insights into Martian dust charging, radio emission properties, and potential implications for planetary exploration. By comparing terrestrial and Martian discharge phenomena, this work contributes to a more comprehensive understanding of dust-driven electrostatic and electromagnetic interactions, which are crucial for future mission planning and atmospheric modeling.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 6","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-07-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145171784","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":"Space Weathering Change of Grain Surfaces using Meteorite Tests and Related Possible Consequences on Asteroid Properties","authors":"A. Kereszturi,&nbsp;I. Gyollai,&nbsp;S. Biri,&nbsp;Z. Juhász,&nbsp;Cs. Király,&nbsp;R. Rácz,&nbsp;D. Rezes,&nbsp;B. Sulik,&nbsp;M. Szabó,&nbsp;Z. Szalai,&nbsp;P. Szávai","doi":"10.1134/S0038094624602081","DOIUrl":"10.1134/S0038094624602081","url":null,"abstract":"<p>Compositional and structural understanding of asteroids, especially the moderately small (and frequent) Near Earth Asteroids is important not only for science but also for possible mitigation against their any future impact. However, space weathering substantially modifies the surface infrared spectra, making it difficult to identify their composition. Laboratory tests of artificial weathering by simulated solar wind on meteorites were conducted and reviewed in this study. During the simulations, an increase in the iron content, amorphization, water loss and other structural changes were observed, which usually decreases the mechanical hardness of the very thin surface layer. Using these results, the question was formulated and evaluated here: could such surface changes influence the joint behavior of grain groups when effects driven by YORP forces modify the global shape of asteroids. Based on the evaluation, 10–100 million years of time scale changes are expected to occur both mineral structure and global asteroid shape. The related theoretical consequences and research questions are summarized here.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 6","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-07-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145171337","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":"The EXO-UV Program: Latest Advances of Experimental Studies to Investigate the Biological Impact of UV Radiation on Exoplanets","authors":"X. C. Abrevaya,&nbsp;P. Odert,&nbsp;M. Leitzinger,&nbsp;O. Oppezzo,&nbsp;G. J. M. Luna,&nbsp;M. R. Patel,&nbsp;A. Hanslmeier","doi":"10.1134/S0038094624602019","DOIUrl":"10.1134/S0038094624602019","url":null,"abstract":"<p>The EXO-UV program is an international, interdisciplinary collaboration between astrophysicists and biologists aimed at expanding the characterization of ultraviolet radiation (UVR) environments on exoplanets. UVR is particularly relevant because it reaches the surface of planets and can influence their habitability. High UVR fluxes emitted during flares and superflares are of particular interest due to the limited information available regarding their biological impact and the lack of experimental studies to evaluate their influence. Our first initial study in the EXO-UV program focused on experimentally studying the potential biological impact of a flare and a superflare on Proxima b, and the second considered a superflare on the TRAPPIST-1 system planets e, f, g. The survival of microorganisms belonging to both the Bacteria and Archaea domains (<i>Deinococcus radiodurans, Pseudomonas aeruginosa, Escherichia coli, Haloferax volcanii</i>) was evaluated. Microorganisms were exposed to UVR (UVC = 254 nm) at fluence rates and fluences equivalent to those they would receive from flares and superflares on the unshielded surfaces of these planets. Our results show the existence of a small fraction of the cell population that can tolerate these high fluences, suggesting that previous research underestimated the ability of “life as we know it” to withstand these high UVR fluxes. These results also document the tolerance of well-known microorganisms to high fluences of UVR related to flares and superflares in quantities and at wavelengths that these microorganisms do not experience on the present Earth.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 6","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-07-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145171296","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":"Motion Properties under Various Perturbations in the Circular Restricted 3-Body Problem","authors":"Abdullah,&nbsp;Majhar Ali,&nbsp;Sonia Aneja,&nbsp;Sada Nand Prasad","doi":"10.1134/S0038094625600040","DOIUrl":"10.1134/S0038094625600040","url":null,"abstract":"<p>The aim of this paper is to investigate the motion properties of the infinitesimal variable mass body under the effects of gravitational forces of the primaries and the Poynting–Robertson drag. The equations of motion are determined for the above said perturbations along with those caused by the second primary having modified Newtonian potential. Utilizing these equations of motion, we analytically evaluate the equilibrium points and their stability as well as reveal the numerical study for potential surfaces, equilibrium points, basins of attractions and the stability of equilibrium points. This study presents useful insights for understanding the impact of various perturbations on the motion of small particles in a system and provides the impetus for innovative research in the field of dynamical astronomy and celestial mechanics.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 6","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-07-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164602","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":"Potential Primary Xenon Components in Nanodiamond-Enriched Fractions of Meteorites: Characteristics of Isolated Components During Oxidation","authors":"A. B. Fisenko,&nbsp;L. F. Semjonova,&nbsp;T. A. Pavlova","doi":"10.1134/S0038094625600155","DOIUrl":"10.1134/S0038094625600155","url":null,"abstract":"<p>To achieve a detailed picture of the isolated potential primary xenon components during stepwise oxidation of nanodiamond-enriched fractions (NDEF) of meteorites, a new isotopically anomalous component Xe-pr3 has been introduced. The peculiarity of this component is a lower value of the ratio ¹³⁴Xe/¹³⁶Xe compared to that component used in (Fisenko et al., 2024b) Xe-pr2n (0.529 versus 0.591, respectively). As a result, the modeling interval of possible values of the ratio ¹³⁴Xe/¹³⁶Xe has increased in anomalous isotopic compositions of isolated xenon. This has led to the possibility of obtaining a complete and detailed picture of the isolated putative xenon components based on the analysis of high-precision data for xenon isolated during stepwise oxidation of LD1 NDEF of the Murchison meteorite (CM2) (Lewis, 1994). Comparative analysis of isolated xenon components using calculated cosmogenic neon contents (²¹Ne_c) showed the following. The relatively low-temperature, nearly isotopically normal Xe-P3 component in NDEF meteorites, identified in (Huss, Lewis, 1994), is contained in an individual carrier phase with low thermal-oxidative stability. This component, according to the authors’ concept, represents a mixture of Xe-P3n with Xe-S in a ratio of 1 : 0.013. The carrier phase of this component is likely to be diamond-like rims. Their surface localization is indicated by the simultaneous release of radiogenic ¹²⁹Xe. The release of isotopically anomalous Xe-pr1n corresponds to the layer-by-layer oxidation of diamond grains. When using SiC-X grains as the carrier phase, the components Xe-pr3 (Fisenko et al., 2024a) its unusual (“explosive”) release (about 70% at one oxidation stage) is explained by us by the formation of surface amorphous films of silicon dioxide on these grains. The assumption about SiC-X grains as a carrier phase of the isotopically anomalous component Xe-pr3 is confirmed by the revealed connection between this component and cosmogenic neon ²¹Ne_c. It is also shown that the “normal” primary component of neon in terms of isotopic composition (designated by us as Ne-P3n) corresponds to the isotopic composition of neon isolated at the high-temperature oxidation stage of LD1 NDEF. Therefore, the isotopic composition of the Ne-P3 component is the result of mixing the primary composition with an additional portion of the isotope ²²Ne (Ne-E) in a ratio of 1 : 0.05. This mixing probably occurred early in the evolution of the protoplanetary cloud of the Solar system. Successful modeling of the isotopic compositions of xenon isolated at almost all stages of the temperature range of oxidation of LD1 NDEF of the Murchison meteorite using a new(?) potentially primary component of xenon in combination with the rest allows us to consider them real and possible when analyzing xenon in NDEF of other meteorites.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 6","pages":""},"PeriodicalIF":0.8,"publicationDate":"2025-07-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164604","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}