Year: 2020
Type: article
Abstract: In our research, we studied 9 eclipsing binary stars: AR Lac, U CrB, S Equ, SU Boo, VV UMa, WW Gem, YY Eri, V0404 Lyr, HP Aur.We collected large sets of moments of minima from BRNO and observational data from AAVSO databases.Then, we obtained the moments of minima for AAVSO observations (totally 397 minima) using the method of approximation with symmetric polynomial, realized in software MAVKA.This software was provided by Kateryna D. Andrych and Ivan L. Andronov.Then, we combined the obtained moments of minima with the data taken from BRNO and plotted OC diagrams.For all the stars, these diagrams represented sinus-like oscillations with the superposition of a linear trend (for SU Boo, VV UMa, WW Gem, V0404 Lyr and HP Aur) or a parabolic trend (for AR Lac, U CrB, S Equ and YY Eri).The oscillations could be described as the presence of the third component, which does not take part in eclipses, but causes the well-known light-time eect (LTE).That eect could be easily detected using long data series of observations.However, the oscillations show clear asymmetry, which we interpreted by an elliptical shape of the third components' orbit.The parabolic trend is explained by a mass transfer between components of a binary system.For all the stars, we computed the minimal possible mass of the third component.In addition, we developed our own code in the computed language Python and, using it, we computed orbital elements of the third component.For the stars with a parabolic trend, we calculated the mass transfer rate.For all computed values, the errors (accuracy) were estimated.
Source: Journal of Physical Studies
DOI: 10.30970/jps.24.3904
Authors: D. E. Tvardovskyi, V. I. Marsakova, I. L. Andronov
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
OpenAlex ID: W2994158498