Solar System Research最新文献

{"title":"Improvement of a Uniaxial Seismic Accelerometer, an Integral Part of the Three-Axis Seismic Accelerometer SEM (ExoMars Seismometer)","authors":"A. B. Manukin,&nbsp;N. F. Sayakina,&nbsp;N. A. Chernogorova,&nbsp;A. K. Ton’shev,&nbsp;I. I. Kalinnikov","doi":"10.1134/S0038094624700308","DOIUrl":"10.1134/S0038094624700308","url":null,"abstract":"<p>A three-axis seismic accelerometer was developed and created, containing three uniaxial mutually perpendicular sensors, the sensitivity axis of each sensor is located at an angle of 54.736° to the local gravitational vertical. For the first time, additional magnetic rigidity has been introduced into each device, allowing the device to be finely tuned to the conditions of a particular planet. However, the accumulated experience in conducting ground-based tests has shown the need to improve the uniaxial seismic accelerometer, which can significantly improve the characteristics of the device. First, we use a single material—beryllium bronze BrB-2—for the manufacture of massive test mass suspension elements with a thickness of 1.5 mm and an elastic element made of a thin strip 10–20 microns thick, which reduces the likelihood of instability. Secondly, we reduce the gap in the capacitors of capacitive converters from 0.25 to 0.1–0.15 mm to significantly increase the conversion slope of the capacitive sensor. Thirdly, we change the technology of setting up the device, for which we combine all the elements of the sensitive part of a uniaxial seismogravimeter using special vertical inserts. This allows us to place the device as a whole in a system for its configuration, eliminating the possibility of failure of individual elements, thereby increasing the reliability of the device.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 4","pages":"404 - 408"},"PeriodicalIF":0.6,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612739","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 Evolutionary State of Near-Earth Comet 7P/Pons–Winnecke","authors":"A. O. Novichonok,&nbsp;A. A. Shmal’ts,&nbsp;S. V. Nazarov,&nbsp;A. S. Pozanenko,&nbsp;E. V. Novichonok,&nbsp;M. A. Tereshina,&nbsp;V. A. Voropaev","doi":"10.1134/S003809462470028X","DOIUrl":"10.1134/S003809462470028X","url":null,"abstract":"<p>7P/Pons–Winnecke is a near-Earth short-period comet of a moderate activity level. In this paper, we present the analysis of observations performed during a favorable apparition of the comet in 2021, indicating its status as a transitional ageing comet. The sublimation starts when the comet is close to the Sun, at a distance of <i>R</i>_ON = 1.76 ± 0.1 AU, and continues for ~13 months, which is apparently caused by residual reserves of water ice. The dust production rate of the comet is not high even at perihelion (&lt;150 kg/s), and the 1.4-percent active portion of the nucleus area is sufficient to provide this mass loss. The photometric age of the comet is <i>P</i>_AGE = 54.4 comet years; being combined with a light curve amplitude of <i>A</i>_SEC(1;1) = 5.5^<i>m</i>, this age corresponds to the state of a transitional middle-aged comet.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 4","pages":"456 - 468"},"PeriodicalIF":0.6,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612741","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":"New Results of Radiation Study on Board TGO ExoMars in 2018–2023","authors":"J. Semkova,&nbsp;V. Bengin,&nbsp;R. Koleva,&nbsp;K. Krastev,&nbsp;Y. Matveychuk,&nbsp;B. Tomov,&nbsp;N. Bankov,&nbsp;S. Malchev,&nbsp;Ts. Dachev,&nbsp;V. Shurshakov,&nbsp;S. Drobyshev,&nbsp;I. Mitrofanov,&nbsp;D. Golovin,&nbsp;A. Kozyrev,&nbsp;M. Litvak,&nbsp;M. Mokrousov","doi":"10.1134/S0038094624700291","DOIUrl":"10.1134/S0038094624700291","url":null,"abstract":"<p>The article provides a brief description of the Liulin-MO dosimeter, which is part of the FREND (Fine Resolution Epithermal Neutron Detector) device installed on the <i>TGO</i> (<i>Trace Gas Orbiter</i>) spacecraft of the <i>ExoMars-2016</i> mission. Since April 2018, <i>TGO</i> has been operating in orbit around Mars. Data are presented on the radiation environment in the orbit of Mars during the decline phase of the 24th cycle of solar activity and the growth phase of the 25th cycle. During the period under review, a maximum flux and dose rate due to galactic cosmic rays (GCR) were observed. Between July 2021 and March 2023, the Liulin-MO dosimeter recorded eight increases in particle fluxes and dose rates from solar proton events (SPEs). Data are presented on the radiation environment during the SPE in Mars orbit in July 2021–March 2022, when Mars was on the opposite side of the Sun from Earth. A comparison is made of particle fluxes measured in orbits around the Earth and Mars.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 4","pages":"367 - 376"},"PeriodicalIF":0.6,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612652","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":"Analysis of Spacecraft Flight Trajectories to Venus with a Flyby of Asteroids","authors":"V. A. Zubko,&nbsp;N. A. Eismont,&nbsp;R. R. Nazirov,&nbsp;K. S. Fedyaev,&nbsp;A. A. Belyaev","doi":"10.1134/S0038094624700163","DOIUrl":"10.1134/S0038094624700163","url":null,"abstract":"<p>We have studied energy-low-cost ballistic trajectories of a spacecraft flight to Venus with asteroid flyby. It is shown that when using schemes including a gravitational maneuver required to deliver the lander to a given area on the surface of Venus, the passing of at least one asteroid is possible. A total of 39 asteroids were discovered, whose passage can occur when launching in 2029–2050. An analysis of the attainable landing areas during the flight of a spacecraft to Venus along trajectories of this type has been performed. It is shown that in each launch window in the period from 2029 to 2050, it is possible to find an asteroid whose passage is possible during the time period between two approaches of the spacecraft to Venus.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 3","pages":"334 - 352"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141119690","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":"Valley Relief of the Northeastern Part of Terra Cimmeria on Mars","authors":"A. E. Mukhamedzhanova","doi":"10.1134/S0038094624700175","DOIUrl":"10.1134/S0038094624700175","url":null,"abstract":"<p>A study of the valley topography of the northeastern part of Terra Cimmeria on Mars was carried out. The results of the study allow us to draw the following conclusions. (1) The morphology of the studied valley systems corresponds to their presumed fluvial origin. (2) The remains of the paleodelta in the Gusev crater, fragments of terrace levels traced along the valley, regular changes in their height, as well as the remains of eroded accumulative bodies discovered in the Ma’adim Valley indicate the existence of individual episodes of partial filling of the valleys with sediment, probably due to the activation of the uppermost links of the valley system that supplied fragmentary material to the main valley. A detailed study of the morphology and topography of the Durius Valley suggests the same mechanism of its formation.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 3","pages":"269 - 275"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141120101","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":"Studying the Dynamics of Multiplets of Orbital Resonances of Asteroids with Small Perihelion Distances","authors":"T. Yu. Galushina,&nbsp;O. N. Letner,&nbsp;O. M. Syusina","doi":"10.1134/S0038094624700151","DOIUrl":"10.1134/S0038094624700151","url":null,"abstract":"<p>The study of orbital resonances in the dynamics of asteroids and major planets is important from the point of view of solving the asteroid hazard problem. In the course of such studies, there is often a need to analyze a large number of time series of resonant (critical) arguments, since to complete the picture it is necessary to consider not only the main argument, but also the entire multiplet. To work with multiplets, we developed an algorithm and program for classifying the behavior of the resonant argument, which were applied to the study of the dynamics of resonant objects with small perihelion distances. The paper presents the results of constructing and analyzing resonance multiplets for 13 such asteroids. The study showed that in order to identify the features of the resonant interaction of the studied asteroids with planets, in most cases it is enough to consider the behavior of the main critical argument. The use of a program to automate the process of classifying the behavior of arguments significantly reduced the time spent and the likelihood of random errors in the process of processing the received data.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 3","pages":"326 - 333"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141121914","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":"An Optically Thin and Thick Dust Exosphere of Active Asteroids: Spectral Signs and Possible Formation Mechanisms","authors":"V. V. Busarev,&nbsp;E. V. Petrova,&nbsp;V. B. Puzin,&nbsp;S. I. Barabanov,&nbsp;M. P. Shcherbina,&nbsp;S. Yu. Kuznetsov","doi":"10.1134/S003809462470014X","DOIUrl":"10.1134/S003809462470014X","url":null,"abstract":"<p>The detection and study of spectral signs of sublimation-driven dust activity (SDA) in 20 primitive-type asteroids of the Main Belt observed in the visible range allowed us to ascertain its temporal (or periodic) character. The asteroids exhibit SDA of relatively low intensity at minimal heliocentric distances, when their subsolar temperatures are, accordingly, highest (i.e., the surface temperature of the asteroid at the center of its sunlit hemisphere is close to the absolute maximum). Most likely, the major cause of SDA in these asteroids is that their interior contains H₂O ice, which becomes outcropped due to recent impact events. As follows from the numerical modeling of the reflectance spectra of active asteroids under consideration, the optically thin dust exosphere (DE), which was induced by SDA and envelopes these bodies, consists of submicron homogeneous particles of different composition and/or fractal-like aggregates of such particles. Taking into account an extremely weak gravitational field of asteroids that cannot hold this optically thin DE even for a short time (especially, if their sizes are less than ~10 km), we conclude that the DE of active primitive-type asteroids is supported by two jointly operating mechanisms. Namely, the electrostatic field of photoemission nature creates a plasma–dust sheath on a sunlit side of the asteroid (as in all atmosphereless celestial bodies), and SDA provides the additional ejection of dust particles from the surface into this layer, which enhances their amount to a detectable level; at the same time, the self-rotation of the body contributes to the spreading of dust around the asteroid.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 3","pages":"315 - 325"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141120558","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":"Impact Structures on Venus as a Result of Asteroid Destruction in the Atmosphere","authors":"V. V. Shuvalov,&nbsp;B. A. Ivanov","doi":"10.1134/S0038094623700089","DOIUrl":"10.1134/S0038094623700089","url":null,"abstract":"<p>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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"163 - 175"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150713","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":"Crater Formed by the Impact of the Luna-25 Spacecraft","authors":"A. T. Basilevsky,&nbsp;B. A. Ivanov,&nbsp;V. P. Dolgopolov","doi":"10.1134/S0038094623700090","DOIUrl":"10.1134/S0038094623700090","url":null,"abstract":"<p>On August 11, 2023, the <i>Luna-25</i> 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 <i>Luna-25</i>, 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 <i>Luna-25</i>. 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 <i>Luna-25</i>. 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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"141 - 147"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150714","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":"Numerical Investigation of Slope Stability in Valles Marineris, Mars","authors":"Yahya Barzegar,&nbsp;Mahnoosh Biglari,&nbsp;Ali Ghanbari","doi":"10.1134/S0038094623600257","DOIUrl":"10.1134/S0038094623600257","url":null,"abstract":"<p>The rock walls of Valles Marineris (VM) valleys on Mars reveal significant gravitational failures, resulting in a sequence of massive landslides spanning several hundred cubic kilometers in volume. For further Mars exploration missions, it is critical to understand which characteristics impact the stability of these rock walls. In this work, ArcGIS is used to identify 30 steep slopes. Utilizing the finite element method, we calculate the proposed seven possibly landslide-prone slopes based on geometry in VM. Using Strength Reduction Method (SRM) in Midas GTS NX, the impacts of variations in cohesion, internal friction angle, unit weight, and elastic modulus of soil and rock on the slope safety factor against landslides are evaluated. The Strength Reduction Method (SRM) is a widely used approach in geotechnical engineering to assess slope stability. It involves systematically reducing the strength parameters of the soil and rock materials within the slope until failure occurs. By iteratively reducing the strength parameters, the SRM calculates the factor of safety against landslides. Internal friction angle is the most critical factor in determining the stability of a slope under low gravity circumstances since it has the widest range of possible alterations. Furthermore, the material’s cohesion and unit weight significantly impact the safety factor, although elastic modulus barely affects slope stability. A modulus of elasticity of more than 35 GPa will not enhance the factor of safety. There is no significant difference in soil suction between Earth and Martian gravities near the surface water table. However, as the groundwater depth increases, soil suction under Martian gravity becomes notably lower than that on Earth. Additionally, consistent with prior investigations, the Vadose zone on Mars is positioned at higher elevations relative to Earth, indicating the presence of a higher capillary fringe. Furthermore, the factor of safety for slope stability consistently outperforms Earth for equivalent slope configurations under unsaturated conditions, with approximately 2.5 times higher factor of safety for higher suctions and approximately 1.5 times higher factor of safety for lower suctions compared to Earth.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 2","pages":"176 - 186"},"PeriodicalIF":0.6,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141150769","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}