Period decrease in three SuperWASP eclipsing binary candidates near the short-period limit

TL;DR

This study analyzes SuperWASP data for 53 contact binary candidates near the short-period limit, finding significant period decreases in three systems likely caused by unstable mass transfer, indicating potential mergers.

Contribution

It provides the first evidence of significant period decreases in contact binaries near the short-period limit, suggesting a new mechanism involving unstable mass transfer.

Findings

Period decreases confirmed in three binaries with high significance.

Period changes are unlikely due to magnetic braking or gravitational radiation.

Systems may merge if period decreases continue.

Abstract

SuperWASP light curves for 53 W UMa-type eclipsing binary (EB) candidates, identified in previous work as being close to the contact binary short-period limit, were studied for evidence of period change. The orbital periods of most of the stars were confirmed, and period decrease, significant at more than 5 sigma, was observed in three objects: 1SWASP J174310.98+432709.6 (-0.055 \pm0.003 s/yr), 1SWASP J133105.91+121538.0 (-0.075 \pm0.013 s/yr) and 1SWASP J234401.81-212229.1 (-0.313 \pm0.019 s/yr). The magnitudes of the observed period changes cannot be explained by magnetic braking or gravitational radiation effects, and are most likely primarily due to unstable mass transfer from primary to secondary components, possibly accompanied by unstable mass and angular momentum loss from the systems. If these period decreases persist, the systems could merge on a relatively short timescale.