THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES
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-p...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | en_US |
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IOP Publishing
2015
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| Online Access: | http://hdl.handle.net/1721.1/93200 https://orcid.org/0000-0003-3182-5569 |
| _version_ | 1811089435672969216 |
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| author | Borkovits, T. Csizmadia, Sz. Kalomeni, B. Tran, Ky-Anh Levine, Alan M Rappaport, Saul A |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Borkovits, T. Csizmadia, Sz. Kalomeni, B. Tran, Ky-Anh Levine, Alan M Rappaport, Saul A |
| author_sort | Borkovits, T. |
| collection | MIT |
| description | 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 M[subscript ☉] yr[superscript –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. |
| first_indexed | 2024-09-23T14:19:08Z |
| format | Article |
| id | mit-1721.1/93200 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T14:19:08Z |
| publishDate | 2015 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/932002022-09-29T08:39:55Z THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES Borkovits, T. Csizmadia, Sz. Kalomeni, B. Tran, Ky-Anh Levine, Alan M Rappaport, Saul A Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Levine, Alan M. Rappaport, Saul A. Tran, K. 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 M[subscript ☉] yr[superscript –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. Szombathely (Hungary) (Agreement S-11-1027) 2015-01-29T18:15:39Z 2015-01-29T18:15:39Z 2013-08 2013-05 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/93200 Tran, K., A. Levine, S. Rappaport, T. Borkovits, Sz. Csizmadia, and B. Kalomeni. “ THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES .” The Astrophysical Journal 774, no. 1 (August 19, 2013): 81. © 2013 The American Astronomical Society https://orcid.org/0000-0003-3182-5569 en_US http://dx.doi.org/10.1088/0004-637x/774/1/81 Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing American Astronomical Society |
| spellingShingle | Borkovits, T. Csizmadia, Sz. Kalomeni, B. Tran, Ky-Anh Levine, Alan M Rappaport, Saul A THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES |
| title | THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES |
| title_full | THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES |
| title_fullStr | THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES |
| title_full_unstemmed | THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES |
| title_short | THE ANTICORRELATED NATURE OF THE PRIMARY AND SECONDARY ECLIPSE TIMING VARIATIONS FOR THE KEPLER CONTACT BINARIES |
| title_sort | anticorrelated nature of the primary and secondary eclipse timing variations for the kepler contact binaries |
| url | http://hdl.handle.net/1721.1/93200 https://orcid.org/0000-0003-3182-5569 |
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