Перегляд за Автор "Kimakovsky, S. R."

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    Observation of an occultation of the UCAC4 488-082551 star by asteroid (76228) 2000 EH 75 on 31 May 2022
    (Одеський національний університет імені І. І. Мечникова, 2022) Gorbanev, Yuriy M.; Kleshchonok, V. V.; Kimakovsky, S. R.; Горбаньов, Юрій Михайлович
    Observations of an occultation of the UCAC4 488-082551 star by asteroid (76228) 2000 EH 75 were carried out on 31 May 2022 at Kryzhanivka observation station of Odesa I. I. Mechnykov National University (the observatory code A85). A set of instruments, which included a Schmidt telescope (the primary mirror diameter D = 271.25 mm; the corrector plate diameter Dk = 223.9 mm; the focal length F = 440 mm), a GPS receiver and Videoscan-415-2001 CCD camera, was used to perform observations. The observing conditions were as follows: clear sky, the star’s altitude 490 south, the Moon was below the local horizon. The target star from the UCAC4 catalogue (Zacharias et al. 2013) has the following photometric parameters: mB = 14.008; mv = 12.720; mr = 12.284; m, = 11.813. The diameter of the star has not been determined. Asteroid (76228) is a Main Belt asteroid with an orbital period of 4.17178 years. It has an absolute magnitude of 14.93, the visible geometric albedo of 0.123±0.013 and diameter of 5.00±0.23 km (Masiero et al. 2011). The time of occultation predicted using ephemerides was 23:52:44±4 sec. The maximum duration of the occultation was 0.4 sec, provided that the observing site was located at the centre of the occultation track (strip). A drop in the star’s brightness observed during occultation was about 8m. The occultation event was recorded as a sequence of GIF images with the exposure time of 0.5 sec per frame. The system clock of the computer used for the occultation recording was controlled with a GPS receiver in a fashion similar to that described in the paper by Karbovsky et al. (2017). The data processing yielded an estimate of the occultation duration of 0.46±0.04 sec. The uncertainty of the occultation start time within exposure results in the total estimate of accuracy in timing the maximum phase of occultation 23:52:44.06±0.10 sec. The chord length across the asteroid estimated by timing the occultation is L = 9.2±0.8. This chord length is close to the estimates of the asteroid diameter reported in the paper by Masiero et al. (2011).
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    POSITIONAL MEASUREMENTS OF THE METEOR TV IMAGES
    (Astroprint, 2010) Gorbanev, Juri M.; Kimakovsky, S. R.; Knyazkova, E. F.
    We discuss the methods and software which is used for processing of the meteor TV images. Methods are based on the principles of the aperture CCD photometry. Software enables one to make processing of the observational material that was secured using TV methods with telescopic systems (field of view less that 1 angular degree), as well as with astrocameras of the wide field of view (field of view less 2-4 angular degrees, and even more than 50 degrees). We also elaborated method that allows one to identify operatively and to measure automatically rectangular coordinates within the image frame, as well as to calculate equatorial coordinates of the object using the Turner method and compiled stellar catalogues. This method was tested with observational material obtained with the help of TV meteor patrol within the period from 2003 to 2010 at Kryzhanovka station that belongs to Astronomical Observatory of Odessa National University. We performed an analysis of accuracy determination of the stellar images measurements. Software was tested in order to use it for the comet observations.
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    Документ
    The effect of major meteor streams on the total ozone in the earth's atmosphere
    (Одеський національний університет імені І. І. Мечникова, 2017) Gorbanev, Juri M.; Stogneeva, I. A.; Shestopalov, V. A.; Knyazkova, E. F.; Kimakovskaya, I. I.; Kimakovsky, S. R.; Golubaev, A. V.
    The correlation between the total ozone and activity of major meteor streams, such as the Perseids, Geminids, Leonids and Orionids, has been found using the Total Ozone Mapping Spectrometer (TOMS) measurements of the global ozone distribution over the periods 1978 􀀀 1993 and 1996 - 2001. The autocorrelation analysis of the total ozone time series for the period of about 20 years has confirmed the existence of regular changes in the ozone levels at the peaks of meteor shower activity. It has been established that TO decreases after the dates of peak activity of meteor streams (e.g. the Perseids) or during the whole periods of meteor shower activity (e.g. the Geminids, Orionids and Leonids). The analysis of the total ozone distribution (in the Southern and Northern Hemispheres), as well as the local distribution of ozone (over the selected surface area of several hundred square kilometres), was performed during the Leonid meteor shower in 1999.