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11.
N. V. Emelyanov M. V. Andreev A. A. Berezhnoi A. S. Bekhteva S. N. Vashkovyak Yu. I. Velikodskii I. A. Vereshchagina D. L. Gorshanov A. V. Devyatkin I. S. Izmailov A. V. Ivanov T. R. Irsmambetova V. A. Kozlov S. V. Karashevich A. N. Kurenya Ya. V. Naiden K. N. Naumov N. A. Parakhin V. N. Raskhozhev S. A. Selyaev A. V. Sergeev E. N. Sokov M. Yu. Khovrichev E. V. Khrutskaya M. M. Chernikov 《Solar System Research》2011,45(3):264-277
In 2009, in five Russian observatories photometric observations of Jupiter’s Galilean satellites during their mutual occultations and eclipses were carried out. Based on these observations, an original method was used to ascertain astrometric results such as the difference between the coordinates of pairs of satellites. Fifty-three phenomena were successfully observed. A total of 94 light curves of satellites were measured. The error in the coordinates of satellites due to random errors in photometry, calculated on all data obtained, was 0.041″ in right ascension and 0.046″ in declination. The discrepancies between the theory and observations in these coordinates was found to be 0.060″ and 0.057″, respectively. The results were uploaded to the common database for all observations of natural satellites of planets at the Natural Satellites Data Center (NSDC), which is available online at http://www.sai.msu.ru/neb/nss/index.htm. For the first time in the practice of photometric observations of satellites in epochs of mutual occultations and eclipses a new method of observation was tested, which eliminates from astrometric results the major systematic errors caused by an inaccurate account of the background level. The tests were conducted in the Terskol Observatory and the observatory of the Crimean laboratory of the Sternberg State Astronomical Institute of the Moscow State University. The application of the new method showed that the elimination of the background level at these observatories was carried out correctly. 相似文献
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I. A. Vereshchagina E. N. Sokov D. L. Gorshanov A. V. Devyatkin V. N. L’vov S. D. Tsekmeister E. S. Romas A. A. Martyusheva 《Solar System Research》2014,48(5):382-390
Astrometric and photometric observations of asteroid (308635) 2005 YU55 were carried out at the computer-aided ZA-320M and MTM-500M telescopes of the Pulkovo observatory in the period of its closest approach to the Earth, from November 9 to 20, 2011. The new orbit of the asteroid changed after its close approach to the Earth was determined. From this orbit, a close approach to Venus on January 19, 2029, was precalculated, and the distance at the closest approach—359000 km—was estimated. From the analysis of the acquired photometric data, the axial rotation period of the asteroid was more accurately determined, and it amounted to 16.3 ± 0.4 h. The color indexes of the asteroid, B-V, V-R, and R-I, were estimated, which allowed the taxonomic class of the asteroid, B, to be determined from them. In addition, from our photometric observations of the asteroid, the earlier unknown change in its brightness with a period of 0.9–1.2 h was detected; the cause of this change has not been completely studied yet. 相似文献
13.
In 2007–2010, ten asteroids were observed in the JHK bands. The color indexes J-H and H-K were determined from the observations. Their positions in the two-color diagram generally correspond to the areas occupied by the asteroids of the corresponding taxonomic types. For two asteroids, (624) Hektor and (762) Pulcova, the light curves in the J and H bands and the curves of the color index J-H were constructed. The changes in the color index J-H from 0.05 m to 0.1 m were revealed; it may be supposed that they are caused by the heterogeneity in structure or mineral composition of the surface. For all of the asteroids, the astrometric positions were obtained. It was found that the best reference catalogue for the astrometric processing of observations of asteroids in the JHK bands under a small field of view is the 2MASS survey. 相似文献
14.
Results from an analysis of a forty year series of photographic observations of the binary star 61 Cyg on the 26 inch refractor
at the Pulkovo Observatory are presented. The orbit is constructed and the sum of the masses of the components is determined
from the relative positions of the components. A study of the individual motions of the components of 61 Cyg relative to the
surrounding stars yields their mass ratio and the masses of the main and secondary components, 0.74 and 0.46 solar masses,
respectively. The relative motion of the components is found to have a fluctuating component with a period of 6.5 years which
may be caused, in particular, by the presence in the system of a dark, low-mass companion.
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Translated from Astrofizika, Vol. 49, No. 3, pp. 453–465 (August 2006). 相似文献
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16.
P. Descamps F. Marchis J. Pollock F. Vachier M. Kaasalainen M.H. Wong E.M. Cooper P. Wiggins M. Polinska A. Devyatkin D. Gorshanov 《Icarus》2008,196(2):578-600
In 2007, the M-type binary Asteroid 22 Kalliope reached one of its annual equinoxes. As a consequence, the orbit plane of its small moon, Linus, was aligned closely to the Sun's line of sight, giving rise to a mutual eclipse season. A dedicated international campaign of photometric observations, based on amateur-professional collaboration, was organized and coordinated by the IMCCE in order to catch several of these events. The set of the compiled observations is released in this work. We developed a relevant model of these events, including a topographic shape model of Kalliope refined in the present work, the orbit solution of Linus as well as the photometric effect of the shadow of one component falling on the other. By fitting this model to the only two full recorded events, we derived a new estimation of the equivalent diameter of Kalliope of 166.2±2.8 km, 8% smaller than its IRAS diameter. As to the diameter of Linus, considered as purely spherical, it is estimated to 28±2 km. This substantial “shortening” of Kalliope, gives a bulk density of 3.35±0.33 g/cm3, significantly higher than past determinations but more consistent with its taxonomic type. Some constraints can be inferred on the composition. 相似文献
17.
A. V. Devyatkin D. L. Gorshanov V. N. L’vov S. D. Tsekmeister M. S. Chubey 《Kinematics and Physics of Celestial Bodies》2016,32(5):241-244
The use of ground-based and space baseline observations of Solar System bodies is considered. Baseline observations allow one to determine the distance to observed objects and (in some cases) the parameters of their orbital motion. Certain results of baseline observations of near-Earth asteroids and the results of model analysis of spacecraft observations are presented. 相似文献
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Pogodin M. A. Pavlovskii S. E. Beskrovnaya N. G. Drake N. A. Kozlova O. V. Alekseev I. Yu. Fenandes M. Borges Pereira C. B. Valyavin G. G. Miroshnichenko A. S. Gorda S Yu. Gorshanov D. L. 《Astrophysics》2022,65(1):31-52
Astrophysics - Results are presented from a spectroscopic study of the Ae/Be Herbig star HD 259431 conducted from 2010 to 2019 using high-resolution spectrographs at: (a) the Crimean Astrophysical... 相似文献
20.
Devyatkin A. V. Gorshanov D. L. Gritsuk A. N. Mel'nikov A. V. Sidorov M. Yu. Shevchenko I. I. 《Solar System Research》2002,36(3):248-259
We present the results of photometric observations of Saturn's seventh satellite Hyperion and four other planetary satellites: Saturn's moon Phoebe and three Jovian satellites Himalia, Elara, and Pasiphae. The observations have been conducted from September, 1999 to March, 2000, and during September–October, 2000. Analysis of periodic variations in Hyperion's lightcurve was performed. The lightcurve was modeled using the software package developed for calculating the rotational dynamics of a satellite. Our data generally indicate that over the period of observations Hyperion was in the chaotic mode of rotation. 相似文献