Orbital period and multi-color light curves ’ investigation of OW Leo are presented for the first time .
The orbital period of OW Leo is corrected from P = 0.325545 days to P = 0.32554052 days in our work , and the observational data from the All-Sky Automated Survey for SuperNovae ( ASAS-SN ) are used to test the newly determined orbital period .
Then , the phased light curves are calculated with the new period and the Wilson-Devinney program is applied to model the light curves , which reveal that OW Leo is a W-subtype shallow contact binary system ( q = 3.05 , f = 12.8 \% ) .
The absolute physical parameters of the two component stars are estimated to be M _ { 1 } = 0.31 ( 1 ) M _ { \odot } , M _ { 2 } = 0.95 ( 3 ) M _ { \odot } , R _ { 1 } = 0.63 ( 1 ) R _ { \odot } , R _ { 2 } = 1.04 ( 1 ) R _ { \odot } , L _ { 1 } = 0.43 ( 1 ) L _ { \odot } and L _ { 2 } = 1.01 ( 2 ) L _ { \odot } .
The evolutionary status show that the more massive star is less evolved than the less massive star .
OW Leo has very low metal abundance , which means its formation and evolution are hardly influenced by any additional component .
It is formed from an initially detached binary systems through nuclear evolution and angular momentum loss via magnetic braking , and have passed a very long time of main sequence evolution .