UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
We compose systems of empirical isochrones for single and binary stars with various components' mass ratio $q=M_{2}/M_{1}$ ($M_{2}$ – mass of the secondary component, $M_{1}$ – mass of the primary component) in order to search for unresolved binaries and multiple stars in open star clusters. We fit an empirical isochrone for single stars across the main sequence (MS) elements assigned using the HDBSCAN algorithm. Isochrones for binaries are obtained by shifting this empirical isochrone to values determined using PARSEC theoretical isochrones. We determine the parameter q for each source that lies within the corresponding intervals between the binary isochrones. We then plot a probability density distribution of the component mass ratio q and estimate the fraction of binaries in the cluster. This work is focuses on the study of close open star clusters with heliocentric distances less than 200 pc. We consider the color-magnitude diagrams (CMDs) in the Gaia photometric system and the two-index diagrams (TIDs) composed of bands in the visible and infrared wavelengths.
open clusters and associations: general; binaries (including multiple): close
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