Orbital period correction and light curve modeling of the W-subtype shallow contact binary OWLeo

TL;DR

This study refines the orbital period of the W-subtype shallow contact binary OW Leo, models its light curves, and estimates the physical parameters of its components, revealing insights into its evolutionary status.

Contribution

The paper provides the first investigation of OW Leo's orbital period and light curves, correcting its period and modeling its physical parameters using the Wilson-Devinney program.

Findings

Orbital period corrected to 0.32554052 days.

OW Leo is a W-subtype shallow contact binary.

Component masses and radii estimated, showing evolutionary insights.

Abstract

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.