• Yu. I. Protsyuk Research Institute “Mykolaiv Astronomical Observatory”, Ukraine
  • N. V. Maigurova Research Institute “Mykolaiv Astronomical Observatory”, Ukraine


Ключові слова:

CCD observations, double and multiple stars, WDS catalog


Double and multiple star systems are the
source of unique information for determining the parame-
ters of star formation models and for testing stellar models
evolution. Therefore observations and measuring of their
mutual configuration parameters is still important.
Observations of double and multiple star systems at the
Research Institute “Mykolaiv Astronomical Observatory”
(RI MAO) were performed with different telescopes since
2013. In addition, we also have an observational database
and proceeding results of the fields in open clusters vicini-
ty, which were performed using the KT-50 telescope
(D=500mm, F=3000mm) in 2011–2020. All astrometric
processing was carried out by the Astrometrica software
using UCAC4 or GAIA DR2 as reference catalogs. The
catalogs of stars positions and proper motions in the vicin-
ity of open clusters that contain more than 5.6 million
stars were created as results of these observations. There
are a lot of double and multiple stars in the fields with
open clusters, which, moreover, could be the physical
member of clusters. With this aim software for search and
measuring of mutual configuration parameters of the dou-
ble and multiple stars from the WDS was created. Our
software uses previous reduction data from Astrometrica
software and allows finding stars from double and multi-
ple systems, which are presented in WDS catalog.
We determined separations and position angles for
pairs of the found WDS systems and checked observa-
tional array over 71 nights of 2019. Data of 9679 CCD
images were reduced and 34277 WDS pairs were found in
7232 of them. Total numbers of unique pairs are 1504 in
1091 systems with average number of pair observations
near 23. The standard errors of measurements were 0.15"
for separations and 0.5° for position angles. The epoch
difference between our observations and the last observa-
tion in the WDS database is in the range from 2 to 28
years. The comparison with the WDS data has shown that
residual differences and their standard errors are
(–0.03±0.24)" in separations and (–0.07±0.88)° in position
angles for close observation periods. The obtained data are
of original observations that extend the observation period
of stars from double and multiple systems and can be used
to construct orbits and to determine the masses of compo-
nents. The calculated parameters of mutual configuration
of the found pairs and estimates of differences in magni-
tudes of the components will be sent to the WDS database


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