Four-color charge-coupled device ( CCD ) light curves in B , V , Rc and Ic bands of the total-eclipsing binary system , V1853 Ori , are presented .
By comparing our light curves with those published by previous investigators , it is detected that the O ’ Connell effect on the light curves is disappeared .
By analyzing those multi-color light curves with the Wilson-Devinney code ( W-D code ) , it is discovered that V1853 Ori is an A-type intermediate-contact binary with a degree of contact factor of f = 33.3 \% ( 3.7 \% ) and a mass ratio of q = 0.1896 ( 0.0013 ) .
Combining our 10 new determined times of light minima together with the others published in the literature , the period changes of the system is investigated .
We found that the general trend of the observed-calculated ( O - C ) curve shows a downward parabolic variation that corresponds to a long-term decrease in the orbital period with a rate of dP / dt = -1.96 ( 0.46 ) \times { 10 ^ { -7 } } d yr ^ { -1 } .
The long-term period decrease could be explained by mass transfer from the more-massive component to the less-massive one .
By combining our photometric solutions with the Gaia DR 2 data , absolute parameters were derived as M _ { 1 } = 1.20 M _ { \odot } , M _ { 2 } = 0.23 M _ { \odot } , R _ { 1 } = 1.36 R _ { \odot } , and R _ { 2 } = 0.66 R _ { \odot } .
The long-term period decrease and the intermediate-contact configuration suggest that V1853 Ori will evolve into a high fill-out overcontact binary .