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

被引:25
作者
Lohr, M. E. [1 ]
Norton, A. J. [1 ]
Kolb, U. C. [1 ]
Anderson, D. R. [2 ]
Faedi, F. [3 ]
West, R. G. [4 ]
机构
[1] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England
[2] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England
[3] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland
[4] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England
关键词
stars: variables: general; binaries: eclipsing; stars: individual: V1067Her; stars: individual: GSC 2314-0530; binaries: close; URSAE-MAJORIS BINARIES; MAGNETIC BRAKING; CONTACT BINARIES; TIME-SERIES; SPACED DATA; EVOLUTION; STARS; LIGHT; MASS;
D O I
10.1051/0004-6361/201219158
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 +/- 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.
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页数:6
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