English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

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. Bycomparing our light curves with those published by previous investigators, itis detected that the O'Connell effect on the light curves is disappeared. Byanalyzing those multi-color light curves with the Wilson-Devinney code (W-Dcode), it is discovered that V1853 Ori is an A-type intermediate-contact binarywith 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 minimatogether with the others published in the literature, the period changes of thesystem is investigated. We found that the general trend of theobserved-calculated $(O-C)$ curve shows a downward parabolic variation thatcorresponds 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 decreasecould be explained by mass transfer from the more-massive component to theless-massive one. By combining our photometric solutions with the Gaia DR 2data, 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 configurationsuggest that V1853 Ori will evolve into a high fill-out overcontact binary.

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