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Tidal Synchronization and Differential Rotation of Kepler Eclipsing Binaries

John C. LurieDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]Karl VyhmeisterDepartment of Astronomy California Institute of Technology, Pasadena, CA 91125, USASuzanne L. HawleyDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]Jamel AdiliaDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]Andrea ChenDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]James R. A. DavenportDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]Mario JurićDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]Michael Puig-HolzmanDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]Kolby L. WeisenburgerDepartment of Astronomy University of Washington, Seattle, WA 98195, USA; [email protected]

2017en

ABI

Annotatsiya

Abstract Few observational constraints exist for the tidal synchronization rate of late-type stars, despite its fundamental role in binary evolution. We visually inspected the light curves of 2278 eclipsing binaries (EBs) from the Kepler Eclipsing Binary Catalog to identify those with starspot modulations, as well as other types of out-of-eclipse variability. We report rotation periods for 816 EBs with starspot modulations, and find that 79% of EBs with orbital periods of less than 10 days are synchronized. However, a population of short-period EBs exists, with rotation periods typically 13% slower than synchronous, which we attribute to the differential rotation of high-latitude starspots. At 10 days, there is a transition from predominantly circular, synchronized EBs to predominantly eccentric, pseudosynchronized EBs. This transition period is in good agreement with the predicted and observed circularization period for Milky Way field binaries. At orbital periods greater than about 30 days, the amount of tidal synchronization decreases. We also report 12 previously unidentified candidate δ Scuti and γ Doradus pulsators, as well as a candidate RS CVn system with an evolved primary that exhibits starspot occultations. For short-period contact binaries, we observe a period–color relation and compare it to previous studies. As a whole, these results represent the largest homogeneous study of tidal synchronization of late-type stars.

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Identifikatorlar

DOI: 10.3847/1538-3881/aa974d

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