Time-series photometric observations were made for the high amplitudeδScuti star CW Ser between 2011 and 2012 at the Xinglong Station of National Astronomical Observatories,Chinese Academy of Sciences.After performing the frequency analysis of the light curves,we confirmed the fundamental frequency of f=5.28677 c d 1,together with seven harmonics of the fundamental frequency,which are newly detected.No additional frequencies were detected.The O C diagram,produced with the 21 newly determined times of maximum light combined with those provided in the literature,helps to obtain a new ephemeris formula of the times of maximum light with the pulsation period of 0.189150355±0.000000003 d.
We present a time-series BV CCD photometry for an EB-type eclipsing binary NSVS 1908107, a member of the young open cluster NGC 869. The photometric solution was obtained by using the 2003 version of the Wilson-Devinney code. It reveals that the system is a semi-detached binary with the secondary component filling its Roche lobe. The mass ratio was determined to be 0.059±0.001. With the physical parameters of the cluster, the masses, radii and luminosities of the two components of NSVS 1908107 are estimated to be M1 = 10.34±2.29 M⊙, R1 = 4.65re±0.34 Rspectivel⊙, L1 = 8076 y. The results s±371 L = 2.40 how tha⊙and M2 = 0.61 t the secondary co±0.13M⊙, R2±0.17 R⊙, L2 = 1054±48 L⊙mponent could be a giant or subgiant star with the outer envelope being stripped.
Data representing 864 times of light maxima of the high-amplitude δ Scuti star CY Aqr were collected from the literature,based on which,long-term period changes of the variable star were investigated.A revised period and new ephemerides were given for the pulsating star.Remarkable cyclic variations were found in the O-C residuals which can be attributed to the light-time effects due to probable unseen components of the object.By using Kopal's method,the orbital parameters of the supposed component stars were derived.The solution suggests that CY Aqr is very probably in a triple system orbited eccentrically by two low-mass companions with periods of 54.2 and 47.3 yr.The lower limits on masses were estimated as0.04 M_⊙and 0.02 M_⊙,respectively,for the two hidden companions.
Photometric observations of AH Cnc,a W UMa-type system in the open cluster M67,were carried out by using the 50 BiN telescope.About 100 h of time-series B- and V-band data were taken,based on which eight new times of light minima were determined.By applying the Wilson-Devinney method,the light curves were modeled and a revised photometric solution of the binary system was derived.We confirmed that AH Cnc is a deep contact(f= 51%),low mass-ratio(q = 0.156) system.Adopting the distance modulus derived from study of the host cluster,we have re-calculated the physical parameters of the binary system,namely the masses and radii.The masses and radii of the two components were estimated to be respectively 1.188(±0.061) M_☉,1.332(±0.063) R_☉ for the primary component and 0.185(±0.032) M_☉,0.592(±0.051) R_☉ for the secondary.By adding the newly derived minimum timings to all the available data,the period variations of AH Cnc were studied.This shows that the orbital period of the binary is continuously increasing at a rate of dp/dt = 4.29×10^(-10)dyr^(-1).In addition to the long-term period increase,a cyclic variation with a period of 35.26 yr was determined,which could be attributed to an unresolved tertiary component of the system.
We present a study on pulsations of the high-amplitudeδScuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory(XAO)and the Xinglong 85-cm telescope of National Astronomical Observatories,Chinese Academy of Sciences(NAOC).Fourier analysis of the light curves reveals the fundamental radial mode and its five harmonics,with the fourth and fifth being newly detected.Thirtynine new times of maximum light are determined from the light curves,and combined with those in the literature,we construct the O-C diagram,derive a new ephemeris and determine a new value for the updated period of 0.104091579(2).In addition,the O-C diagram reveals an increasing rate of period change for YZ Boo.Theoretical models are calculated and constrained with the observationally determined parameters of YZ Boo.The mass and age of YZ Boo are hence derived as M=1.61±0.05 M_⊙ and age=(1.44±0.14)×10~9 yr,respectively.With both the frequency of the fundamental radial mode and the rate of period change,YZ Boo is located at the post main sequence stage.
Tao-Zhi YangAli EsamdinJian-Ning FuHu-Biao NiuGuo-Jie FengFang-Fang SongJin-Zhong LiuLu Ma
