The use of the EPOS software package for research of the solar system objects

L'Vov, V. N.; Tsekmeister, S. D.

doi:10.1134/s0038094612020074

Cited by 30 publications

(2 citation statements)

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“…The last correction was calculated using preliminary Linus orbit constructed without any corrections. For the correction to positional angle, the ephemerides of 22 Kalliope asteroid were calculated using EPOS software package [L'vov, Tsekmeister, 2012] with the asteroid orbital elements shared by E.Bowell (ftp://ftp.lowell.edu/pub/elgb/astorb.html). The corrections for the phase angle were calculated using Lambert's cosine law for spherical body [Toulmonde et al, 1994].…”

Section: Determination Of Linus' Apparent Orbital Parametersmentioning

confidence: 99%

The binary Asteroid 22 Kalliope: Linus orbit determination on the basis of speckle interferometric observations

Sokova

Sokov

Roschina

et al. 2014

Icarus

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In this paper we present the orbital elements of Linus satellite of 22 Kalliope asteroid. Orbital element determination is based on the speckle interferometry data obtained with the 6meter BTA telescope operated by SAO RAS. We processed 9 accurate positions of Linus orbiting around the main component of 22 Kalliope between 10 and 16 December, 2011. In order to determine the orbital elements of the Linus we have applied the direct geometric method. The formal errors are about 5 mas. This accuracy makes it possible to study the variations of the Linus orbital elements influenced by different perturbations over the course of time. Estimates of six classical orbital elements, such as the semi-major axis of the Linus orbit a = 1109 ± 6 km, eccentricity e = 0.016 ± 0.004, inclination i = 101° ± 1° to the ecliptic plane and others, are presented in this work.

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Section: Determination Of Linus' Apparent Orbital Parametersmentioning

confidence: 99%

The binary Asteroid 22 Kalliope: Linus orbit determination on the basis of speckle interferometric observations

Sokova

Sokov

Roschina

et al. 2014

Icarus

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“…The second, EPOS, provides independent ephemeris support, checkout of observations and estimation of their accuracy. It helps in objects identification, orbits determination and improvement, modeling the objects apparent motion on the sky and orbital motion in space (L'vov, Tsekmeister (2012)). Its recent facility -studying the motion of Troyan, Horseshoe and Quasi-satellite asteroids.…”

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confidence: 99%

Near Earth Objects Research in Pulkovo Observatory

Devyatkin¹,

Bashakova²,

Gorshanov³

et al. 2012

Proc. IAU

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More than 20000 observations of Near Earth asteroids and comets are collected and reduced in Pulkovo Observatory during last 10 years. For observations of these objects two robotic telescopes are used -ZA-320M (Cassegrain system, D = 320 mm, F = 3200 mm) at Pulkovo and MTM-500M (Maksutov -Cassegrain system, D = 500 mm, F = 4100 mm) at Kislovodsk mountain station. These telescopes perform CCD observations of objects up to 18.0 and 20.5 magnitude, correspondingly. The results of observations are regularly submitted to Minor Planet Center.Two software packages developed in Pulkovo observatory are now in practice. The first one, APEX, is used for automatic CCD frame processing (Devyatkin et al. (2010)). The second, EPOS, provides independent ephemeris support, checkout of observations and estimation of their accuracy. It helps in objects identification, orbits determination and improvement, modeling the objects apparent motion on the sky and orbital motion in space (L'vov, Tsekmeister (2012)). Its recent facility -studying the motion of Troyan, Horseshoe and Quasi-satellite asteroids.Several NEAs were observed in the frame of GAIA FUN-SSO program. The Near Earth asteroid 2005 YU55 has approached to Venus, Earth and Mars. The EPOS software helped to model the sharp changes of its orbit during the close approaches. It was observed with ZA-320M and MTM-500M telescopes during its close approach to the Earth in November 2012. 926 positions with mean accuracies of 0".1 − 0".4 were obtained, results were sent to Minor Planet Center. Using the observations the asteroid orbit was improved. From its light-curves the period of rotation was estimated and the color-indices in BV RI system were determined. To estimate the period (using Scargles method) all our observations which were made without filter were processed. The value of 16.3 hr was obtained, while the value determined earlier with radar observations is 18 hr (see http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=308635).During processing the data, one more period was noticed in observations made with both telescopes in several nights. Its value varies from 0.9 to 1.2 hr for different nights. The magnitude range is about 0.15 m . The long-time observations (≈ 10 hr) include several period durations. If this period is real, it could meant that the asteroid is binary.The weighted means of color-indices from our observations are the following:Our value of V − R color-index is in agreement with the effective color (V − R = 0.37 m ) measured from spectrum of the asteroid in works Hicks et al. (2011a), Hicks et al. (2011b).We have tried to classify 2005 YU55 asteroid using our wide-band photometry. Dandy et al. (2003) classify asteroids on Tholens classification using wide-band photometry: BV RI and additional Z band at 0.91μm. We have no Z filter. But using their method 472 https://www.cambridge.org/core/terms. https://doi

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