V0405 Dra:A New Deep and Low Mass Ratio Contact Binary with Extremely Fast Decrease in the Orbital Period  

作　　者：Chao-Yue Li Lin-Qiao Jiang Jie Zheng Yi-Man Liu Xiao-Yu Long Min Sun Han-Lu Zhang Xiao-Man Tian 

机构地区：[1]School of Science,Leshan Normal University,Leshan 614000,China [2]Center for Applied Optics Research,Leshan Normal University,Leshan 614000,China [3]Key Laboratory of Detection and Application of Space Effect in Southwest Sichuan,Leshan 614000,China [4]CAS Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [5]School of Aeronautics,Shandong Jiaotong University,Jinan 250000,China

出　　处：《Research in Astronomy and Astrophysics》2024年第6期287-293,共7页天文和天体物理学研究（英文版）

基　　金：supported by the Joint Research Fund in Astronomy(grant No.U1631108)under a cooperative agreement between the National Natural Science Foundation of China(NSFC);the Chinese Academy of Sciences(CAS);the Chinese National Natural Science Foundation of China(NSFC,grant No.12103030)。

摘　　要：V0405 Dra is a W UMa-type binary star.Based on the TESS data,we have conducted an orbital period study and performed a light curve analysis for the system.The orbital period study reveals that the O-C curve for V0405 Dra exhibits secular decrease at an extremely high rate of d P/dt=-2.71×10^(-6)day year^(-1),along with periodic variations characterized by an amplitude of A_(3)=0.0032 day and a period of P_(3)=1.413 years.The orbital periodic change is possibly due to the light-travel time effect resulting from an additional third body in the system,for which we estimate a minimum mass of M_(3)=0.77M_(⊙).By employing the 2013 version of the Wilson-Devinney(W-D)method to synthesize a light curve,we derived photometric solutions indicating that V0405 Dra is a new deep(f=68.7%)and low-mass ratio(q=0.175)contact binary.The fast decrease in its orbital period is likely caused by mass transfer from the more massive primary star to the less massive secondary star,or due to angular momentum loss.With further mass transfer and loss of angular momentum,the binary will gradually evolve into a tighter contact configuration,eventually leading to a merger into a single star,following the evolutionary paths suggested for such deep and low mass ratio contact binaries.

关 键 词：(stars:)binaries(including multiple):close (stars:)binaries:eclipsing stars:individual(V0405 Dra) 

分 类 号：P153[天文地球—天文学]