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https://hdl.handle.net/11147/5162
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DC Field | Value | Language |
---|---|---|
dc.contributor.author | Tran, K. | - |
dc.contributor.author | Levine, A. | - |
dc.contributor.author | Rappaport, S. | - |
dc.contributor.author | Borkovits, T. | - |
dc.contributor.author | Csizmadia, Sz. | - |
dc.contributor.author | Kalomeni, Belinda | - |
dc.date.accessioned | 2017-03-28T12:29:18Z | |
dc.date.available | 2017-03-28T12:29:18Z | |
dc.date.issued | 2013-09 | |
dc.identifier.citation | Tran, K., Levine, A., Rappaport, S., Borkovits, T., Csizmadia, S.,and Kalomeni, B. (2013). The anticorrelated nature of the primary and secondary eclipse timing variations for the kepler contact binaries. Astrophysical Journal, 774(1). doi:10.1088/0004-637X/774/1/81 | en_US |
dc.identifier.issn | 0004-637X | |
dc.identifier.issn | 0004-637X | - |
dc.identifier.uri | https:doi.org/10.1088/0004-637X/774/1/81 | |
dc.identifier.uri | http://hdl.handle.net/11147/5162 | |
dc.description.abstract | We report a study of the eclipse timing variations in contact binary systems, using long-cadence lightcurves from the Kepler archive. As a first step, observed minus calculated (O-C) curves were produced for both the primary and secondary eclipses of some 2000 Kepler binaries. We find ∼390 short-period binaries with O-C curves that exhibit (1) random walk-like variations or quasi-periodicities, with typical amplitudes of ±200-300 s, and (2) anticorrelations between the primary and secondary eclipse timing variations. We present a detailed analysis and results for 32 of these binaries with orbital periods in the range of 0.35 ± 0.05 days. The anticorrelations observed in their O-C curves cannot be explained by a model involving mass transfer, which, among other things, requires implausibly high rates of ∼0.01 MȮ yr-1. We show that the anticorrelated behavior, the amplitude of the O-C delays, and the overall random walk-like behavior can be explained by the presence of a starspot that is continuously visible around the orbit and slowly changes its longitude on timescales of weeks to months. The quasi-periods of ∼50-200 days observed in the O-C curves suggest values for k, the coefficient of the latitude dependence of the stellar differential rotation, of ∼0.003-0.013. | en_US |
dc.description.sponsorship | TUBITAK (112T776); City of Szombathely (S-11-1027) | en_US |
dc.language.iso | en | en_US |
dc.publisher | IOP Publishing Ltd. | en_US |
dc.relation.ispartof | Astrophysical Journal | en_US |
dc.rights | info:eu-repo/semantics/openAccess | en_US |
dc.subject | Stars | en_US |
dc.subject | Binaries | en_US |
dc.subject | Eclipsing | en_US |
dc.subject | Kepler archive | en_US |
dc.title | The Anticorrelated Nature of the Primary and Secondary Eclipse Timing Variations for the Kepler Contact Binaries | en_US |
dc.type | Article | en_US |
dc.authorid | TR17457 | en_US |
dc.institutionauthor | Kalomeni, Belinda | - |
dc.department | İzmir Institute of Technology. Physics | en_US |
dc.identifier.volume | 774 | en_US |
dc.identifier.issue | 1 | en_US |
dc.identifier.wos | WOS:000323426700081 | en_US |
dc.identifier.scopus | 2-s2.0-84883091928 | en_US |
dc.relation.publicationcategory | Makale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı | en_US |
dc.identifier.doi | 10.1088/0004-637X/774/1/81 | - |
dc.relation.doi | 10.1088/0004-637X/774/1/81 | en_US |
dc.coverage.doi | 10.1088/0004-637X/774/1/81 | en_US |
dc.identifier.wosquality | Q1 | - |
dc.identifier.scopusquality | Q1 | - |
item.fulltext | With Fulltext | - |
item.openairetype | Article | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
Appears in Collections: | Physics / Fizik Scopus İndeksli Yayınlar Koleksiyonu / Scopus Indexed Publications Collection WoS İndeksli Yayınlar Koleksiyonu / WoS Indexed Publications Collection |
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