New Photometric Investigation of the Low-Mass-Ratio Contact Binary Star V1853 Orionis

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.