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dc.contributor.authorRappaport, S.
dc.contributor.authorDeck, K.
dc.contributor.authorLevine, A.
dc.contributor.authorBorkovits, T.
dc.contributor.authorCarter, J.
dc.contributor.authorEl Mellah, I.
dc.contributor.authorSanchis-Ojeda, R.
dc.contributor.authorKalomeni, Belinda
dc.date.accessioned2017-04-12T07:51:42Z
dc.date.available2017-04-12T07:51:42Z
dc.date.issued2013-05
dc.identifier.citationRappaport, S., Deck, K., Levine, A., Borkovits, T., Carter, J., El Mellah, I., Sanchis-Ojeda, R., and Kalomeni, B. (2013). Triple-star candidates among the Kepler binaries. Astrophysical Journal, 768(1). doi:10.1088/0004-637X/768/1/33en_US
dc.identifier.issn0004-637X
dc.identifier.urihttp://doi.org/10.1088/0004-637X/768/1/33
dc.identifier.urihttp://hdl.handle.net/11147/5290
dc.description.abstractWe present the results of a search through the photometric database of Kepler eclipsing binaries looking for evidence of hierarchical triple-star systems. The presence of a third star orbiting the binary can be inferred from eclipse timing variations. We apply a simple algorithm in an automated determination of the eclipse times for all 2157 binaries. The "calculated" eclipse times, based on a constant period model, are subtracted from those observed. The resulting O-C (observed minus calculated times) curves are then visually inspected for periodicities in order to find triple-star candidates. After eliminating false positives due to the beat frequency between the ∼1/2 hr Kepler cadence and the binary period, 39 candidate triple systems were identified. The periodic O-C curves for these candidates were then fit for contributions from both the classical Roemer delay and so-called physical delay, in an attempt to extract a number of the system parameters of the triple. We discuss the limitations of the information that can be inferred from these O-C curves without further supplemental input, e.g., ground-based spectroscopy. Based on the limited range of orbital periods for the triple-star systems to which this search is sensitive, we can extrapolate to estimate that at least 20% of all close binaries have tertiary companions. © 2013. The American Astronomical Society. All rights reserved..en_US
dc.description.sponsorshipNASA by the Space Telescope Science Institute (HF-51267.01-A); NASA (NAS 5-26555)en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionof10.1088/0004-637X/768/1/33en_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.subjectBinariesen_US
dc.subjectStarsen_US
dc.subjectKepler binariesen_US
dc.subjectCelestial mechanicsen_US
dc.subjectEclipsingen_US
dc.titleTriple-star candidates among the Kepler binariesen_US
dc.typearticleen_US
dc.contributor.authorIDTR17457en_US
dc.contributor.iztechauthorKalomeni, Belinda
dc.relation.journalAstrophysical Journalen_US
dc.contributor.departmentİYTE, Fen Fakültesi, Fizik Bölümüen_US
dc.identifier.volume768en_US
dc.identifier.issue1en_US
dc.identifier.wosWOS:000317960500033
dc.identifier.scopusSCOPUS:2-s2.0-84876805799
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US


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