Solar System Research最新文献

{"title":"The Flight to Neptune and its Moons Triton and Nereid as a Demonstration of the Possibility of using Low-Thrust Engines in Missions to Giant Planets","authors":"N. A. Simbirev,&nbsp;A. A. Sukhanov,&nbsp;O. L. Starinova","doi":"10.1134/S0038094624601932","DOIUrl":"10.1134/S0038094624601932","url":null,"abstract":"<p>The paper suggests a possible scenario of a flight to Neptune’s moons Triton and Nereid. At the moment, Triton and Nereid remain among the least studied moons in Solar system. A detailed study of Triton can confirm a number of theories about its origin. The study of Nereid, the third largest satellite of Neptune with the greatest eccentricity among all known moons, will help to better understand the evolution of the Neptune moon system and confirm or refute the hypothesis that Triton was captured by Neptune’s gravity and seriously destroyed the original system of its moons. A significant problem in the study of giant planets and their satellites is the lack of effective space transport systems that allow delivering a large payload over such long distances. One of the most promising solutions to this problem is the use of propulsion systems with low thrust, ensuring the implementation of the flight with minimal expenditure of the working fluid. The scenario allows a spacecraft with low-thrust engines to reach Neptune by performing two gravity assist maneuvers near Earth and one gravity assist maneuver near Jupiter. The flyby of Triton and Nereid is carried out within the framework of one mission and make possible to explore the surface of both moons from a distance of 10 thousand km. The achievement of this task is carried out by using a modern ion propulsion system with a specific impulse of 3500 s and a thrust of 0.15 N. It is shown that with an initial mass of 850 kg and a mission duration of 29 years, the total cost of the propellant will not exceed 350 kg.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100303","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":"On the Possible Associations of Sporadic Meteors with Near-Earth Asteroids","authors":"Yu. D. Medvedev,&nbsp;S. R. Pavlov","doi":"10.1134/S0038094624602123","DOIUrl":"10.1134/S0038094624602123","url":null,"abstract":"<p>In this paper, a method for selecting potential rubble pile near-Earth asteroids (NEAs) is proposed. The method is based on statistical analysis of the number of asteroid associations with sporadic meteors from the Global Meteor Network (GMN) database, as well as the value of the of the minimum orbital distance between the Earth and the asteroid (MOID), its magnitude, and the rotation period. The number of associations was calculated for each asteroid i.e., the number of meteors with relatively close meteoroids’ orbits. To determine associations between NEAs and meteors, well known orbital dissimalrity criteria (D-criteria) were used: Southworth and Hawkins, Drummond criteria and Kholshevnikov metric. A meteor was associated with an asteroid if the D-criteria values between their orbits did not exceed selected thresholds. The method is based on the assumption that the proportion of associations in which meteors are genetically related to the asteroid in qestion is significant relative to the total number of associations. With that in mind, we impose a number of constraints regarding the orbits and the rotation periods of the NEAs. A table of asteroids with the largest number of associations which satisfy the imposed restrictions is provided. These asteroids are recommended for further study using polarimetric, photometric and other types of observations to verify whether they belong to the rubble pile type or not. We stress the importance of considering the distribution of the number of associations by dates, depending on the Earth’s orbital position, when moving on to the consideration of individual asteroids.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100302","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":"Radar Mapping of the South Polar Region of the Moon at 4.2 cm Wavelength","authors":"Y. S. Bondarenko,&nbsp;D. A. Marshalov,&nbsp;S. R. Pavlov,&nbsp;A. L. Tolstoy","doi":"10.1134/S003809462460210X","DOIUrl":"10.1134/S003809462460210X","url":null,"abstract":"<p>The paper presents new radar maps of the south polar region of the Moon at 4.2 cm wavelength with an average spatial resolution of 90 m. The maps are based on radar images obtained in 2023 using the 64-m TNA-1500 antenna of the Bear Lakes Satellite Communications Center of the Special Design Bureau of the Moscow Power Engineering Institute and the 13.2-m RT-13 radio telescopes at the Svetloe and Zelenchukskaya observatories of the Institute of Applied Astronomy of the Russian Academy of Sciences. Radar images are formed in a specific coordinate system relating the Doppler frequency shift with the propagation time delay of the echo components, which makes it difficult to tie them to selenographic coordinates. In this paper, an original method for converting echo Doppler frequency and time delay to selenographic latitude and longitude is proposed, using bilinear interpolation by ephemeris nodal values, taking into account long integration times. The accuracy of the reference of the maps constructed in this way was assessed and compared with the LROC WAC global optical map of the Moon and mosaics of permanently shadowed regions from LROC NAC. It is shown that radar maps at 4.2 cm wavelength contain features of the lunar surface that are hidden in optical images and are located in the regolith at depths of up to 1 m or in permanently shadowed regions of the south polar region of the Moon. The maps of the lunar echoes specular and diffuse polarization components, as well as a map of the distribution of circular polarization ratios, are available on the Internet at http://luna.iaaras.ru/ and can be useful for studying the geological history of the Moon, searching for ice deposits, and selecting safe landing sites when planning future lunar missions.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100375","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":"A Simplified Geometrical Approach to Calculation of Solar Eclipses of a Planet’s Satellite in Solving Practical Problems of Venus Exploration","authors":"V. A. Zubko,&nbsp;A. A. Belyaev,&nbsp;N. A. Eismont,&nbsp;K. S. Fedyaev,&nbsp;A. G. Toporkov","doi":"10.1134/S0038094624602135","DOIUrl":"10.1134/S0038094624602135","url":null,"abstract":"<p>This study is focused on the problem of determining the position of a satellite at entry to and exit from the planet’s penumbra with the use of an analytical equation in the closed form. The approach taken is based on the geometric representation of the second-order curve that appeared when the plane of the satellite orbit cuts the conical surface formed by the intersection of sunlight rays and the boundaries of a central body. The time moments of the satellite’s entry to the penumbra and umbra of the planet are determined from the intersection of this curve with the satellite orbit. Based on these ideas, an analytical method for determining the duration of eclipses of a satellite by a planet has been developed. Its application to the analysis of the orbits of an artificial satellite of Venus has been demonstrated. It is ascertained that the method simplifies the search for orbits, the parameters of which satisfy the requirements for the duration of the shadow segment. It is shown that the method can be extended to the solution of the problem of determining the moments of time, at which the satellite passes the region obscured by the planetary atmosphere. It is illustrated on provided examples that the proposed approach can be applied to solving practically important problems in the study of Venus and its atmosphere.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100300","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":"Construction of Transfer Trajectories of the Spacecraft to Asteroids Passing Near Sun-Earth Libration Points","authors":"M. V. Pupkov,&nbsp;N. A. Eismont,&nbsp;O. L. Starinova,&nbsp;K. S. Fedyaev","doi":"10.1134/S0038094624602020","DOIUrl":"10.1134/S0038094624602020","url":null,"abstract":"<p>The paper considers the issues of designing transfer trajectories of spacecraft moving along bounded orbits in vicinities of Sun–Earth libration points to the Near-Earth asteroids Apophis and 2001 WN₅. The study was conducted for the James Webb Space Telescope and the Spectrum–Roentgen–Gamma spacecraft operating near the <i>L</i>₂ Sun–Earth libration point. It is shown that these spacecraft can be transferred to trajectories of a close approach to the target celestial bodies at low fuel costs. The results of numerical calculations of the values of the characteristic velocity required for such flights with the subsequent return of the spacecraft to the vicinity of the initial libration point in order to continue the main mission are presented. The advantage of the proposed concept for the design of flight schemes to Near-Earth asteroids is that all sections of the spacecraft trajectories are located in a vicinity of the Earth.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100305","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":"Some Characteristic Features of Latitudinal Variations in Methane and Ammonia Absorption on Jupiter","authors":"V. D. Vdovichenko,&nbsp;A. M. Karimov,&nbsp;P. G. Lysenko,&nbsp;V. G. Teifel,&nbsp;V. A. Filippov,&nbsp;G. A. Kharitonova","doi":"10.1134/S0038094624601750","DOIUrl":"10.1134/S0038094624601750","url":null,"abstract":"<p>This paper examines the latitudinal variations in the intensity of methane and ammonia absorption bands in the near IR region of the spectrum (600–950 nm), such as CH₄ (619, 703, 727, 780, 861, 889 nm) and NH₃ (645, 790 nm). The results are presented as variations in the profiles of each of the absorption bands, their residual intensities, central depths and equivalent widths both in values obtained directly during the processing of spectrograms and in relation to the reference detail, as well as in relation to each other. The shallowest methane band at 703 nm and the deepest methane band at 886 nm give almost mirror-opposite values of absorption change along Jupiter’s central meridian. The extreme absorption values (maximum for 703 nm and minimum for 890 nm) coincide and fall on the boundary of the Equatorial Zone (EZ) and the Northern Equatorial Belt (NEB) at a relative distance of the radius of the planet’s disk <i>r</i>/<i>R</i> = 0.07. The remaining absorption bands of methane, as their intensity changes, occupy an intermediate position. As in previous years, a clearly expressed local decrease in the intensity of the NH₃ absorption bands is observed and especially centered at 787 nm at the boundary between the Equatorial Zone (EZ) and the North Equatorial Belt (NEB) compared to other regions of the central meridian. The decrease in absorption in this band begins almost from the equator, and its maximum occurs at the planetographic latitude of 10° N, then the absorption increases again, approaching the latitude of 20° N. The NH₃ absorption band at a wavelength of 645 nm also shows a decrease at low latitudes in the northern hemisphere. In the temperate latitudes of the Northern Hemisphere, absorption in this band is systematically lower than in the Southern Hemisphere. A comparison of the authors’ observations with data in the IR region and in the radio range is given, which show that the closest relationship between the brightness temperature and the absorption depth at 890 nm is observed in the upper stratosphere, in the latitude range of ±60°. Good agreement is also observed between the results of our estimates of the meridional absorption variations in the ammonia bands at 645 and 787 nm and the brightness temperature measurements performed at the VLA in the millimeter thermal emission range at frequencies of 8–12 GHz. The data for the 787-nm band in the wake region of the Great Red Spot are in particularly good agreement.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100345","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 Connection Between the April Chi Librids Meteor Shower and Near-Earth Asteroids","authors":"M. V. Sergienko,&nbsp;Yu. A. Nefedyev,&nbsp;A. O. Andreev","doi":"10.1134/S0038094624602032","DOIUrl":"10.1134/S0038094624602032","url":null,"abstract":"<p>The paper examines the April chi Librids meteor shower, which is a minor meteor shower with an unidentified parent body. According to the IAU Meteor Data Center, the April chi Librids meteor shower is registered under number 140. A search for its genetic connections with near-Earth asteroid groups was conducted using an author-modified synthetic method. As a result of establishing genetic links between the April chi Librids meteor shower and near-Earth asteroids of the Apollo group, the following parent bodies were identified: 2013 YC, 2015 DU180, 2011 BT59, and 2013 WM. For the identified parent bodies, an analysis of the discovered genetic relationships was conducted using various methods.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100304","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":"Variations in F10.7 by New Dates of Maximum Meteor Streams","authors":"A. V. Tertyshnikov","doi":"10.1134/S003809462460166X","DOIUrl":"10.1134/S003809462460166X","url":null,"abstract":"<p>During the periods of meteor shower maxima in 2019–2023, small variations in the intensity of solar radiation were noted (<i>F</i>_10.7) in fractions of a percent of the background, calculated in a sliding 5-day window. Estimates of variations in the normalized <i>F</i>_10.7 according to the “old” (before 2006) dates of meteor showers. With the transition to new dates of meteor shower maxima, variations in magnetic activity indices disappeared. The filtering effect of meteoric dust on the regulation of variations in solar UV radiation has been proven. An increase in the intensity of UV radiation on the dates of maxima of strong meteor showers has been confirmed by measurements in 2019 at the Russian Antarctic station Novolazarevskaya.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 5","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144100296","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":"Efficient Techniques to Cope with Chaotic Dynamics in Deterministic Systems","authors":"Pablo M. Cincotta,&nbsp; Claudia M. Giordano","doi":"10.1134/S0038094624601828","DOIUrl":"10.1134/S0038094624601828","url":null,"abstract":"<p>In this work we review and improve two useful techniques to cope with chaotic dynamics in deterministic systems, namely the Mean Exponential Growth factor of Nearby Orbits (MEGNO) and the Shannon entropy. The MEGNO provides a direct measure of the hyperbolic dynamics in an arbitrary small neighborhood of a given point of the phase space in comparatively short motion times and the maximum Lyapunov exponent (or its spectrum) can be easily derived from this fast dynamical indicator which has become a wide-spread tool in the investigation of the global dynamics in planetary systems. The time derivative of the Shannon entropy yields a confident measure of the diffusion speed in comparison with the usual approach of the action-like variance evolution. It has been successfully applied in different dynamical systems, particularly, in exoplanetary systems. A brief discussion concerning the relationship among the Shannon entropy and the Kolmogorov–Sinai or metric entropy and the topological entropy is also addressed. Both methods allow to get two relevant timescales in chaotic dynamics, the Lyapunov time and the diffusion time. An application to a simple 4D symplectic map illustrates the efficiency of both techniques.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 4","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143944216","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":"Algorithms for Computing Hamiltonian Normal Form","authors":"A. G. Petrov,&nbsp;A. B. Batkhin","doi":"10.1134/S0038094624601853","DOIUrl":"10.1134/S0038094624601853","url":null,"abstract":"<p>The invariant normalization method proposed by V.F. Zhuravlev, used for calculating normal or symmetrized forms of autonomous Hamiltonian systems, is discussed. The normalizing canonical transformation is represented by a Lie series using a generating Hamiltonian. This method has a generalization proposed by A.G. Petrov, which normalizes not only autonomous but also nonautonomous Hamiltonian systems. The normalizing canonical transformation is represented by a series using a parametric function. For autonomous Hamiltonian systems, the first two approximation steps in both methods are the same, and the remaining steps are different. The normal forms of both methods are identical. A method for testing a normalization program has also been proposed. For this purpose, the Hamiltonian of a strongly nonlinear Hamiltonian system is found, for which the normal form is a quadratic Hamiltonian. The normalizing transformation is expressed in terms of elementary functions.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"59 4","pages":""},"PeriodicalIF":0.6,"publicationDate":"2025-05-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143944218","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}