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

¹ Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
e-mail: Marcus.Lohr@open.ac.uk
² Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK
³ Astrophysics Research Centre, Main Physics Building, School of Mathematics & Physics, Queen’s University, University Road, Belfast BT7 1NN, UK
⁴ Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK

Received: 2 March 2012
Accepted: 3 May 2012

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 5σ, was observed in three objects: 1SWASP J174310.98+432709.6 (−0.055 ± 0.003 s yr^-1), 1SWASP J133105.91+121538.0 (−0.075 ± 0.013 s yr^-1) and 1SWASP J234401.81−212229.1 (−0.313 ± 0.019 s yr^-1). 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.