Solar System Research最新文献

{"title":"Sublimation-Driven Dust Activity of Primitive-Type Asteroids as a Sign of the Presence of Н2О Ice","authors":"V. V. Busarev,&nbsp;E. V. Petrova,&nbsp;M. P. Shcherbina,&nbsp;M. A. Burlak,&nbsp;N. P. Ikonnikova,&nbsp;M. V. Maksimova","doi":"10.1134/S0038094624700503","DOIUrl":"10.1134/S0038094624700503","url":null,"abstract":"<p>In the period December 12, 2022, to February 28, 2023, we performed a series of <i>UBVRI</i> observations of 65 asteroids, including 50 primitive-type objects, which could be observed near perihelion at that time, and calculated their approximated reflectance spectra. The observations were aimed at searching for spectral signs of sublimation-driven dust activity in the asteroids and formation of a transient dust exosphere, which are caused by the presence of Н₂О ice in their interior and the highest subsolar temperature. Based on the analysis of the accuracy and shape of approximated reflectance spectra of the primitive-type asteroids, a set of which was conventionally restricted by the geometric albedo value not exceeding 0.10, we found sublimation-driven dust activity in asteroids 164 Eva, 360 Carlova, and 750 Oskar by distinct short-term variations in the reflectance of these asteroids in the <i>U</i> band. During one of the nights, similar spectral changes and sublimation-driven dust activity related to them were detected in asteroid 629 Bernardina; the geometric albedo of this asteroid is somewhat higher (0.14 or 0.19), which may be indicative of a heterogeneous composition of its material and, apparently, a local outcropping of water ice on its surface. Moreover, in three asteroids of a high-temperature type, 757 Portlandia, 1121 Natascha, and 1687 Glarona, noticeable variations were detected in the entire spectral range; they may be connected with ejection of submicron dust particles from the surface by some other mechanisms. To substantiate and interpret the results of observations, we numerically modeled the reflectance spectra of conditional asteroids of taxonomic types C and S (with low- and high-temperature mineralogy, respectively), which are enveloped by an optically thin dust exosphere containing aggregate or homogeneous submicron particles of different composition. On the basis of this modeling, we introduce a quantitative criterion to identify a weak sublimation-driven dust activity in primitive-type asteroids in the visible range.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 6","pages":"715 - 731"},"PeriodicalIF":0.6,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142438725","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":"Effects of Modified Potential and Quantum Correction in the Generalized Perturbed Interacting CR3BP with Variable Mass","authors":"Abdullah,&nbsp; Majhar Ali","doi":"10.1134/S0038094624601385","DOIUrl":"10.1134/S0038094624601385","url":null,"abstract":"<p>The aim of this paper is to investigate the motion properties of the infinitesimal body under the effects of gravitational forces, the quantum correction, variable mass, modified Newtonian force, interaction between bodies, triaxial parameters, Coriolis and centrifugal forces in the restricted three-body configuration. Using Jeans law, Meshcherskii space-time transformations and the above perturbations, we evaluate the equations of motion and quasi-Jacobian integral. And then, we numerically illustrate the locations of equilibrium points, regions of motion, Poincare surfaces of section, basins of attraction, periodic orbits and stability of the equilibrium points.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 6","pages":"745 - 758"},"PeriodicalIF":0.6,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142438719","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":"Determination of Variation Lines and Modeling of Initial Trajectory Dispersion in the Presence of Strong Nonlinearity in Orbit Improvement Problems","authors":"A. P. Baturin","doi":"10.1134/S0038094624600951","DOIUrl":"10.1134/S0038094624600951","url":null,"abstract":"<p>A method for determining the lines of variation (LOV) in the initial confidence region under strong nonlinearity in the orbit improvement problem is developed, based on finding the maximum modulus of the normal vector to the level surfaces of the objective function using the least-squares method. The method was tested for three asteroids using their observations on a short arc of the orbit, namely, the points of two variation lines corresponding to the directions of the greatest deformation of the initial confidence region were determined. Approximation of variation lines was performed using third-degree polynomials. Using the obtained approximations, new variables were introduced in which the initial confidence region is almost ellipsoidal, i.e., nonlinearity is nearly absent. The modeling of the initial probability dispersion of trajectories is performed in the space of new variables. The resulting dispersion can be further used to identify collision orbits and estimate the probability of asteroid collisions with Earth.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 6","pages":"759 - 768"},"PeriodicalIF":0.6,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142438720","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":"Study of the Dynamical Evolution of the Compact Planetary System Kepler-51","authors":"E. D. Kuznetsov,&nbsp;A. S. Perminov","doi":"10.1134/S0038094624700394","DOIUrl":"10.1134/S0038094624700394","url":null,"abstract":"<p>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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"594 - 611"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177749","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 Photocenter Shift Phenomenon in Positional Observations of Active Asteroids (6478) Gault and (248370) 2005 QN173/433Р","authors":"S. R. Pavlov,&nbsp;Yu. A. Chernetenko","doi":"10.1134/S0038094624700412","DOIUrl":"10.1134/S0038094624700412","url":null,"abstract":"<p>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).</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"586 - 593"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177747","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":"Propagation of Hydromagnetic Disturbance Waves and Gravitational Instability in a Magnetized Rotating Heat-Conducting Anisotropic Plasma","authors":"A. V. Kolesnichenko","doi":"10.1134/S0038094624700382","DOIUrl":"10.1134/S0038094624700382","url":null,"abstract":"<p>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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"549 - 560"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177745","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 Craters on Earth with a Diameter of More than 200 km: Numerical Modeling","authors":"B. A. Ivanov","doi":"10.1134/S0038094624700370","DOIUrl":"10.1134/S0038094624700370","url":null,"abstract":"<p>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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"509 - 525"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1134/S0038094624700370.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177539","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":"On the Nature of Electrophone Phenomena Accompanying the Passage of Meteoric Bodies through the Earth’s Atmosphere","authors":"A. D. Filonenko","doi":"10.1134/S0038094624700424","DOIUrl":"10.1134/S0038094624700424","url":null,"abstract":"<p>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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"561 - 577"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177746","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":"Determining Optimal Parameters for Mercury’s Magnetospheric Current Systems from MESSENGER Observations","authors":"A. S. Lavrukhin,&nbsp;I. I. Alexeev,&nbsp;D. V. Nevsky","doi":"10.1134/S0038094624700400","DOIUrl":"10.1134/S0038094624700400","url":null,"abstract":"<p>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.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"526 - 536"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177743","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":"Astrometry and Photometry of Potentially Dangerous Asteroid 65690 (1991 DG)","authors":"A. V. Devyatkin,&nbsp;D. L. Gorshanov,&nbsp;V. N. Lvov,&nbsp;S. D. Tsekmeister,&nbsp;S. N. Petrova,&nbsp;A. A. Martyusheva,&nbsp;K. N. Naumov","doi":"10.1134/S0038094624700369","DOIUrl":"10.1134/S0038094624700369","url":null,"abstract":"<p>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: <i>P</i> = 4.3193 ± 0.0028 h.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":"58 5","pages":"578 - 585"},"PeriodicalIF":0.6,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142177750","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}