Observations and light curve solutions of the W UMa binaries V796 Cep,V797 Cep,CSS J015341.9+381641 and NSVS 3853195

查看全文 作　　者：Diana Petrova [1]Kjurkchieva;Velimir Angelov [1,2]Popov;Sunay Ibryamov [1]Ibryamov;Doroteya Lyubenova [1]Vasileva;Nikola Ivanov [3]Petrov 机构地区：[1]Department of Physics,Shumen University,115 Universitetska Str.,9712 Shumen,Bulgaria;[2]IRIDA Observatory,Rozhen NAO,Bulgaria;[3]Institute of Astronomy and NAO,Bulgarian Academy of Sciences,72 Tsarigradsko Shose Blvd.,1784 Sofia,Bulgaria 出　　处：《Research in Astronomy and Astrophysics》索引2017年第17卷第5期,共8页 基　　金：supported partly by grants ND08/20 and RD 08-102 of the Fund for Scientific Research of the Bulgarian Ministry of Education and Science;funded by the National Aeronautics;Space Administration and the National Science Foundation;supported partly by funds from project RD 02–81 of Shumen University 摘　　要：Photometric observations in Sloan g′and i′bands of four W UMa binaries, V796 Cep,V797 Cep, CSS J015341.9+381641 and NSVS 3853195, are presented. Our observations showed that CSS J015404.1+382805 and NSVS 3853195 are the same star. We determined the initial epochs T_0 of all targets and found improved values for the period of NSVS 3853195. The light curve solutions of our data revealed that the components of each target are almost the same in terms of mass, temperature,radius and luminosity. The stellar components are G and K spectral types and undergo partial eclipses.All systems have barely-overcontact configurations and can be classified as H subtype W UMa binaries.We established that the relation between the luminosity ratio l_2/l_1 and mass ratio q of our targets is approximately l_2/l_1 = q^(1.5). 关 键 词：stars:binaries:eclipsing stars:fundamental parameters stars:individual(V796 Cep,V797 Cep,CSS J015341.9+381641,NSVS 3853195)