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Analysis of TESS field Eclipsing Binary Star V948 Her: A Pulsating or Non-pulsating Star?

Research in Astronomy and Astrophysics 2022年第1期22卷 137-147页

作者： f kahraman alicavus O Ekinci Canakkde Onsekiz Mart University Faculty of Sciences and ArtsPhysics Department17100QanakkaleTurkey Canakkale Onsekiz Mart University Astrophysics Research Center and Ulupinar ObservatoryTR-17100CanakkaleTurkey Canakkale Onsekiz Mart University School of Graduate StudiesDepartment of Space Sciences and TechnologiesTR-17100CanakkaleTurkey

Pulsating stars occupy a significant place in the H-R diagram and it was thought that all stars inside the classical instability strip should pulsate. However, recent studies showed that there are many non-pulsating stars located inside the classical instability strip. The existence of these non-pulsating stars is still a mystery. To deeply understand the properties of these non-pulsating and pulsating stars, one needs precise fundamental stellar parameters(e.g. mass).for this purpose, the eclipsing binaries are unique systems. Hence, in this study, we present the TESS data analysis of one candidate pulsating eclipsing binary system, V948 Her. TESS data were used for the binary modeling with the literature radial velocity measurements, and the precise fundamental parameters of the system were obtained. The system’s age was derived as 1 ± 0.24 Gyr. The positions of the binary components in the H-R diagram were examined and the primary component was found inside the δ Scuti instability strip. However, in the frequency analysis of TESS data, we found no significant pulsation frequencies. Only the harmonics of the orbital periods were obtained in the analysis. Therefore, the system was classified as a non-pulsator. V948 Her is an important object to understand the nature of non-pulsating stars inside the δ Scuti instability strip.

关键词： (stars:)binaries:eclipsing stars:fundamental parameters techniques:photometric

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The evolutionary status of chemically peculiar eclipsing binary star DV Boo

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Research in Astronomy and Astrophysics 2020年第9期20卷 309-318页

作者： filiz kahraman alicavus f.alicavus Canakkale Onsekiz Mart University Faculty of Sciences and ArtsPhysics Department17100CanakkaleTurkey Nicolaus Copernicus Astronomical Center Bartycka 18PL-00-716 WarsawPoland

Eclipsing binary systems are unique stellar objects to examine and understand stellar evolution and *** to these systems,the fundamental stellar parameters(mass,radius)can be obtained very *** existence of metallic-line(Am)stars in binaries is noticeably ***,the known number of Am stars in eclipsing binaries is *** Am stars in eclipsing binaries are extremely useful to deeply investigate the properties of Am stars,as eclipsing binaries are the only tool to directly derive the fundamental stellar ***,the atmospheric parameters and metallicities of such binary components could be obtained by a detailed spectroscopic ***,in this study,we present a comprehensive photometric and spectroscopic analysis of the eclipsing binary system DV Boo which has a possible Am *** fundamental stellar parameters were determined by the analysis of radial velocity and photometric light *** atmospheric parameters of both binary components of DV Boo were derived considering the disentangled *** chemical abundance analysis was carried out as *** a result,we showed that the primary component exhibits a typical Am star chemical abundance *** fundamental stellar parameters of the binary components were also obtained with an accuracy offor masses andfor *** evolutionary status of DV Boo was examined utilizing the precisely obtained stellar *** age of the system was found to be 1.00±0.08 Gyr.

关键词： techniques photometric spectroscopic-stars variables binaries eclipsing fundamental parameters-stars individual DV Boo

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Spectroscopic and photometric studies of a candidate pulsating star in an eclipsing binary:V948 Her

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Research in Astronomy and Astrophysics 2018年第7期18卷 133-144页

作者： filiz kahraman alicavus faculty of Sciences and Arts Physics DepartmentCanakkale Onsekiz Mart University17100CanakkaleTurkey

Eclipsing binary stars with a pulsating component are powerful tools that allow us to probe the stellar interior structure and the evolutionary statuses with a good accuracy. Therefore, in this study, spectroscopic and photometric examinations of an eclipsing binary system V948 Her are presented. The primary component of the system is classified to be a candidate 3 Scuti variable in the literature. The fundamental stellar, atmospheric and orbital parameters, and the surface abundance of the star were determined and the pulsation behaviour was investigated in this study. The orbital parameters were derived by the analysis of radial velocity and SuperWASP light curves. The spectral classification was found to be f2V. The initial atmospheric parameters of the primary component were derived by analysis of the spectral energy distribution and hydrogen lines. The final atmospheric parameters and chemical abundances of the primary component were obtained by using the method of spectrum synthesis. As a result, the final atmospheric parameters were determined as Teff= 7100±200 K, log 9= 4.34±0.1 cgs and ζ = 2.2 4± 0.2 km s^-1. The surface abundance was found to be similar to solar. The fundamental stellar parameters of both components were also obtained to be M = 1.722 4±0.123, 0.762 4± 0.020 Me, R = 1.655 4± 0.034,M,R= 0.689 ± 0.016 R for primary and secondary components, respectively. The pulsation characteristic of the primary component was examined using SuperWASP data and the pulsation period was found to be ~0.038 d. The position of the primary pulsating component was also obtained inside the instability strip of δ Sct stars. The primary component of V948 Her was defined to be a Sct variable.

关键词： techniques photometric spectroscopic-stars binaries eclipsing-stars variables δScuti-stars individual(V948 Her)

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