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

作     者：F Kahraman Alicavus O Ekinci F Kahraman Alicavus;? Ekinci

作者机构：Canakkde Onsekiz Mart UniversityFaculty of Sciences and ArtsPhysics Department17100QanakkaleTurkey Canakkale Onsekiz Mart UniversityAstrophysics Research Center and Ulupinar ObservatoryTR-17100CanakkaleTurkey Canakkale Onsekiz Mart UniversitySchool of Graduate StudiesDepartment of Space Sciences and TechnologiesTR-17100CanakkaleTurkey 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2022年第22卷第1期

页      面：137-147页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：supported by the Scientific and Technological Research Council (TUBITAK) project through 120F330 Funding for the TESS mission is provided by the NASA Explorer Program national institutions,in particular the institutions participating in the Gaia Multilateral Agreement 

主　　题：(stars:)binaries:eclipsing stars:fundamental parameters techniques:photometric 

摘      要：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.