Effects of the Mass Transfer and Presence of the  Third Components in Close Binary Stellar Systems

Tvardovskyi, D. E.; Marsakova, V. I.; Андронов, И. Л.

doi:10.18524/1810-4215.2017.30.115463

Cited by 5 publications

(3 citation statements)

References 14 publications

(25 reference statements)

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“…In addition we are grateful to Andrych et al who provided us their software MAVKA for obtaining moments of minima [43], [44], [45]. This research was done as the part of the projects Inter-Longitude Astronomy [49], UkrVO [50] and AstroInformatics [51], [52] as well as previous research [53], [54], [55]. Special acknowledgments to Leonid Shakun for constructive discussion about algorithm of the Python program.…”

Section: Acknowledgmentsmentioning

confidence: 98%

Third components with elliptical orbits in the eclipsing binaries

Tvardovskyi,

Marsakova,

Andronov

2019

Preprint

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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 moments of minima for AAVSO observations (totally -397 minima) using method of approximation with symmetric polynomial, realized in software MAVKA. This software was provided by Kateryna D. Andrych and Ivan L. Andronov. After we combined obtained moments of minima with data taken from BRNO and plotted O-C diagrams. For all stars these diagrams represented sinusoidal-like oscillations with superposition of linear (for SU Boo, VV UMa, WW Gem, V0404 Lyr and HP Aur) or parabolic trend (for AR Lac, U CrB, S Equ and YY Eri). The oscillations could be described as presence of the third component, which does not take part in eclipses, but causes the well-known light-time effect (LTE). That effect could be easily detected using long data series of observations. However, the oscillations have clear asymmetry, which we interpreted as elliptical shape of the third components orbit. Parabolic trend we explained as mass transfer between components of binary system. For all stars we computed minimal possible mass of the third component. In addition, we developed our own code in computed language Python and using it we computed orbital elements of the third component. Moreover, for stars with parabolic trend we calculated rate of the mass transfer. Finally, for all computed values we estimated errors.В нашому дослiдженнi ми вивчили 9 затемнюваних подвiйних зорь: AR Lac, U CrB, S Equ, SU Boo, VV UMa, WW Gem, YY Eri, V0404 Lyr, HP Aur. Ми зiбрали великi масиви мiнiмумiв iз BRNO та спостережень iз бази даних AAVSO. Потiм ми отримали моменти мiнiмумiв для спостережень AAVSO (всього -397 мiнiмумiв) за допомогою методу апроксимацiї з симетричним полiномом, реалiзованого в програмi MAVKA. Це програмне забезпечення надали Катерина Д. Андрич та Iван Л. Андронов. Пiсля того ми поєднали отриманi моменти мiнiмумiв iз даними, отриманими з BRNO, та побудували дiаграми O-C. Для всiх зорь цi дiаграми представляли собою подiбнi до синусоїдальних коливання з суперпозицiєю лiнiйного (для SU Boo, VV UMa, WW Gem, V0404 Lyr та HP Aur) або параболiчного тренду (для AR Lac, U CrB, S Equ та YY Eri). Коливання можна описати як наявнiсть третього компонента, який не бере участi в затемненнях,

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Section: Acknowledgmentsmentioning

confidence: 98%

Third components with elliptical orbits in the eclipsing binaries

Tvardovskyi,

Marsakova,

Andronov

2019

Preprint

Self Cite

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“…MAVKA was already used in several articles: Savastru et al (2017); Tvardovskyi et al (2017Tvardovskyi et al ( , 2018; Andrych et al (2020). In these papers we used the AAVSO observations of different observers.…”

Section: Real Observationsmentioning

confidence: 99%

MAVKA: Investigation of stellar brightness extrema approximation stability for various methods

Andrych¹,

Tvardovskyi²,

Chinarova³

et al. 2020

caosp

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We developed the software package MAVKA for the determination of characteristics of extrema (moment of extremum, magnitude) and their errors. The program realizes the application of 11 basic functions for approximation of extrema. We tested all these methods in two parts. In the first part we used generated data sets (various smooth curves with noise). We investigated deviations between generated and computed values of moments of extremum and magnitude, as well as execution time for different extrema parameters. In the second part we used real observations of different variable stars using photometric and visual observations from different databases.

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“…The original photometric observations were distributed into intervals near extremum and then analyzed with MAVKA. Tvardovskyi et al (2017) studied effects of the Mass Transfer and Presence of the Third Components in Close Binary Stellar Systems. Tvardovskyi et al (2018) detected period variations and possible third components in the eclipsing binaries AH Tauri and ZZ Cassiopeiae.…”

Section: Eclipsing Binary Systemsmentioning

confidence: 99%

Astroinformatics: Statistically Optimal Approximations of Near-Extremal Parts with Application to Variable Stars

Андронов

Andrych

Chinarova

et al. 2020

ComBAO

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The software MAVKA is described, which was elaborated for statistically optimal determination of the characteristics of the extrema of 1000+ variable stars of different types, mainly eclipsing and pulsating. The approximations are phenomenological, but not physical. As often, the discovery of a new variable star is made on time series of a single-filter (single-channel) data, and there is no possibility to determine parameters needed for physical modelling (e.g. temperature, radial velocities, mass ratio of binaries). Besides classical polynomial approximation "AP" (we limited the degree of the polynomial from 2 to 9), there are realized symmetrical approximations (symmetrical polynomials "SP", "wall-supported" horizontal line "WSL" and parabola "WSP", restricted polynomials of non-integer order based on approximations of the functions proposed by Andronov (2012) and Mikulasek (2015) and generally asymmetric functions (asymptotic parabola "AP", parabolic spline "PS", generalized hyperbolic secant function "SECH" and "log-normal-like" "BSK"). This software is a successor of the "Observation Obscurer" with some features for the variable star research, including a block for "running parabola" "RP" scalegram and approximation. Whereas the RP is oriented on approximation of the complete data set. MAVKA is pointed to parts of the light curve close to extrema (including total eclipses and transits of stars and exoplanets). The functions for wider intervals, covering the eclipse totally, were discussed in Andronov (2017). Global and local approximations are reviewed in Andronov (2020). The software is available at http://uavso.org.ua/mavka and https://katerynaandrych.wixsite.com/mavka. We have analyzed the data from own observations, as well as from monitoring obtained at ground-based and space (currently, mainly, TESS) observatories. It may be used for signals of any nature.

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Effects of the Mass Transfer and Presence of the Third Components in Close Binary Stellar Systems

Cited by 5 publications

References 14 publications

Third components with elliptical orbits in the eclipsing binaries

Third components with elliptical orbits in the eclipsing binaries

MAVKA: Investigation of stellar brightness extrema approximation stability for various methods

Astroinformatics: Statistically Optimal Approximations of Near-Extremal Parts with Application to Variable Stars

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