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Семинар Малые тела Солнечной системы (25.11.2020, 13:00)

Опубликовано: 23/11/2020

1. Authors: Anna Kartashova, Alexander Golubaev, AlonaMozgova, Galina Bolgova, Ivan Chuvashov, Dmitry Glazachev, Vladimir Efremov (Institute of Astronomy, Russian Academy of Sciences, Institute of Astronomy of V.N. KarazinKharkiv National University, Astronomical Observatory, Taras Shevchenko Kyiv National University, Institute of Dynamics of Geospheres, Russian Academy of Sciences)


Abstract: In the morning of June 21 2018 (1:16 Universal Time (UTC)) the space body entered the Earth atmosphere in the Lipetsk region, Russia. This event was detected by a number of registration systems in cars, satellite observations of
bolide light curve and subsequent dust trail. The videos, photos, satellite data allow us to calculate the trajectory and the orbit of the Ozerki bolide. The characteristics were analyzed: trajectory, entry velocity and angle, orbit parameters. The mass and the size were estimated. The found material was called Ozerki meteorite and classified as an ordinary chondrite (L6).

2. Authors: Zolotarev R. V. (SFU),

Abstract:  Despite the apparent long-term (billions of years) stability of the Solar system, the population of near-Earth asteroids (NEAs) changes rapidly, on a short time scale (millions of years). This is important not only from a scientific point of view, but also for assessing the age-old variations in the degree of asteroid-comet hazard.Using numerical approach we examine evolution of the population near-Earth asteroids (NEAs) at scale of 10 Myr. The rate of depletion is examined. It is demonstrated that the characteristic time of depletion of the current NEA population is about 5Myr, which is consistent with the estimates given in the literature. This imposes restrictions on the mechanisms for replenishing the population of the NEAs. (based on the results of the publication Zolotarev R. V., Shustov B. M., Korchagin V. I.)

3. Authors: Shematovich V.I., Bisikalo D.V.
Abstract: Studying auroras in the atmospheres of planets and small bodies in the Solar system is a fundamental problem because the auroral phenomena are the prominent manifestation of solar/stellar forcing on planetary atmospheres and are closely related to the energy deposition by and evolution of planetary atmospheres. Observations of auroras are widely used to analyze the composition, structure, and chemistry of the atmosphere under study, as well as charged particle and energy fluxes that affect the atmosphere. Simulation of the processes of solar/stellar wind plasma precipitation into the upper atmospheres of planets and small bodies in the Solar and extrasolar planetary systems has been carried out at the Institute of Astronomy of the Russian Academy of Sciences for the past 20 years. Numerical kinetic Monte Carlo models had been developed that allow us to study the processes of precipitation of high-energy electrons, protons and hydrogen atoms into the planetary atmospheres. Such models allow us to investigate the precipitation processes on molecular level of description with taking into account the stochastic nature of collisional scattering at high kinetic energies, and are used to study auroras at both magnetized and non-magnetized planets in the Solar system. In this report we will present the current status of the kinetic model applications aimed to understand and interpret the auroral emission observations in the upper Martian atmosphere of Mars and to compare with observations by ESA Mars Express and NASA MAVEN spacecrafts.

4. Authors: N. S. Bakhtigaraev, P. A. Levkina – INASAN

Abstract: Regular observations of space debris (SD) are conducted at the Terskol Observatory of TF INASAN using the Zeiss 2000 telescope. 4 observation sessions were held in 2020 on the scientific topics “Astronomy in the Elbrus
region” and “Space threats”. The report presents some results of research on the topics “Study of the population of the geostationary zone of near-earth space with small fragments of SD and “Study of the features of the translational-rotational movement of SD”.

1. Previously unobserved objects from the 18th to the 21st magnitude were found. In particular, for the first time, a fragment of the 20th magnitude was observed on several nights, which was catalogued in the dynamic database of space objects of the Keldyshinsttute under the number 71113.
Previously, such objects were observed, but not catalogued due to insufficient number of measurements. The parameters of the orbit and the brightness change diagram are given.
2. For the first time in December 2019 one SD object was found to have a change in brightness of the same amplitude, the same duration, and the same shape with a period equal to sidereal day. In September 2020 the same changes were detected on the same section of the trajectory. A similar feature of the change in brightness was found in the observations of 2018 too.

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