Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions

作     者：Hu-Biao Niu Jian-Ning Fu Jia-Xin Wang Chun-Qian Li Hu-Biao Niu;Jian-Ning Fu;Jia-Xin Wang;Chun-Qian Li

作者机构：Department of AstronomyBeijing Normal UniversityBeijing 100875China Xinjiang Astronomical ObservatoryChinese Academy of SciencesUrumqi 830011China Key Laboratory of Optical AstronomyNational Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space ScienceUniversity of Chinese Academy of SciencesBeijing 100049China 

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：174-188页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 070402[理学-天体测量与天体力学] 0704[理学-天文学] 

基　　金：the support from the National Natural Science Foundation of China (NSFC) through the grants 11833002, 12090040, and 12090042 Guo Shou Jing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences Funding for the project has been provided by the National Development and Reform Commission LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences Funding for the Kepler mission is provided by the NASA Science Mission directorate 

主　　题：(stars:)binaries:eclipsing (stars:)starspots stars:individual(KIC 8098300) 

摘      要：The LAMOST spectra and Kepler light curves are combined to investigate the detached eclipsing binary KIC 8098300,which shows the O’Connell effect caused by spot/facula *** radial velocity(RV)measurements are derived by using the tomographic spectra disentangling *** mass ratio q=K1/K2=0.812±0.007,and the orbital semimajor axis a sin i=14.984±0.048 R_(⊙)are obtained by fitting the RV *** optimize the binary model concerning the spot/facula activity with the code PHOEBE and obtain precise parameters of the orbit including the eccentricity e=0.0217±0.0008,the inclination i=87°.71±0°.04,and the angle of periastronω=284°.1±0°.*** masses and radii of the primary and secondary star are determined as M_(1)=1.3467±0.0001 M_(⊙),R_(1)=1.569±0.003 R_(⊙),and M_(2)=1.0940±0.0001 M_(⊙),R_(2)=1.078±0.002 R_(⊙),*** ratio of temperatures of the two component stars is r_(teff)=0.924±*** also obtain the periastron precession speed of 0.000024±0.000001 day *** residuals of out-of-eclipse are analyzed using the auto-correlation function and the discrete Fourier *** spot/facula activity is relatively weaker,but the lifetime is longer than that of most single main sequence stars in the same temperature *** average rotation period of the spots P_(rot)=4.32 days is slightly longer than the orbital period,which may be caused by either the migration of spots/faculae along the longitude or the latitudinal differential *** activity may be spot-dominated for the secondary star and facula-dominated for the primary *** method of this work can be used to analyze more eclipsing binaries with the O’Connell effect in the Kepler field to obtain the precise parameters and investigate the difference of spot behavior between binaries and single *** is helpful for a deeper understanding of the stellar magnetic activity and dynamo theory.