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http://hdl.handle.net/20.500.12386/25926
Title: | Detection of Solar-like Oscillations, Observational Constraints, and Stellar Models for θ Cyg, the Brightest Star Observed By the Kepler Mission | Authors: | Guzik, J. A. Houdek, G. Chaplin, W. J. Smalley, B. Kurtz, D. W. Gilliland, R. L. Mullally, F. Rowe, J. F. Bryson, S. T. Still, M. D. Antoci, V. Appourchaux, T. Basu, S. Bedding, T. R. Benomar, O. Garcia, R. A. Huber, D. Kjeldsen, H. Latham, D. W. Metcalfe, T. S. Pápics, P. I. White, T. R. Aerts, C. Ballot, J. Boyajian, T. S. Briquet, M. Bruntt, H. Buchhave, L. A. Campante, T. L. CATANZARO, Giovanni Christensen-Dalsgaard, J. Davies, G. R. Doğan, G. Dragomir, D. Doyle, A. P. Elsworth, Y. FRASCA, Antonio Gaulme, P. Gruberbauer, M. Handberg, R. Hekker, S. Karoff, C. Lehmann, H. Mathias, P. Mathur, S. Miglio, A. Molenda-Żakowicz, J. Mosser, B. Murphy, S. J. Régulo, C. RIPEPI, Vincenzo Salabert, D. Sousa, S. G. Stello, D. Uytterhoeven, K. |
Issue Date: | 2016 | Journal: | THE ASTROPHYSICAL JOURNAL | Number: | 831 | Issue: | 1 | First Page: | 17 | Abstract: | θ Cygni is an F3 spectral type magnitude V = 4.48 main-sequence star that was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were first obtained during Quarter 6 (2010 June-September) and subsequently in Quarters 8 and 12-17. We present analyses of solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 modes with frequencies of 1000-2700 μHz, a large frequency separation of 83.9 ± 0.4 μHz, and maximum oscillation amplitude at frequency ν <SUB>max</SUB> = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, combined with interferometric angular diameter measurements, give T <SUB>eff</SUB> = 6697 ± 78 K, radius 1.49 ± 0.03 R <SUB>☉</SUB>, [Fe/H] = -0.02 ± 0.06 dex, and log g = 4.23 ± 0.03. We calculate stellar models matching these constraints using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses of 1.35-1.39 M <SUB>☉</SUB> and ages of 1.0-1.6 Gyr. θ Cyg’s T <SUB>eff</SUB> and log g place it cooler than the red edge of the γ Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The pulsation models show γ Dor gravity modes driven by the convective blocking mechanism, with frequencies of 1-3 cycles per day (11 to 33 μHz). However, gravity modes were not seen in Kepler data; one signal at 1.776 cycles per day (20.56 μHz) may be attributable to a faint, possibly background, binary. | URI: | http://hdl.handle.net/20.500.12386/25926 | URL: | https://iopscience.iop.org/article/10.3847/0004-637X/831/1/17 | ISSN: | 0004-637X | DOI: | 10.3847/0004-637X/831/1/17 | Bibcode ADS: | 2016ApJ...831...17G | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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Guzik_2016_ApJ_831_17.pdf | Pdf editoriale | 5.39 MB | Adobe PDF | View/Open |
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