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DETECTION OF SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, AND STELLAR MODELS FOR theta CYG, THE BRIGHTEST STAR OBSERVED BY THE KEPLER MISSION

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  • J. A. Guzik, Los Alamos Natl Lab, Los Alamos National Laboratory, United States Department of Energy (DOE), XTD NTA
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  • G. Houdek
  • W. J. Chaplin, Univ Birmingham, University of Birmingham, Sch Phys & Astron
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  • B. Smalley, Keele Univ, Keele University, Astrophys Grp, Sch Phys & Geog Sci, Lennard Jones Labs
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  • D. W. Kurtz, Univ Cent Lancashire, University of Central Lancashire, Jeremiah Horrocks Inst
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  • R. L. Gilliland, Penn State Univ, Penn State University, Pennsylvania Commonwealth System of Higher Education (PCSHE), Ctr Exoplanets & Habitable Worlds
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  • F. Mullally, NASA, Ames Research Center, National Aeronautics & Space Administration (NASA), SETI Inst, Ames Res Ctr
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  • J. F. Rowe, NASA, Ames Research Center, National Aeronautics & Space Administration (NASA), SETI Inst, Ames Res Ctr
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  • S. T. Bryson, NASA, Ames Research Center, National Aeronautics & Space Administration (NASA), SOFIA Sci Ctr, USRA, Ames Res Ctr
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  • M. D. Still, Bay Area Environm Res Inst
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  • V. Antoci
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  • T. Appourchaux, Univ Paris Saclay, Centre National de la Recherche Scientifique (CNRS), University of Paris Sud - Paris XI, Universite Paris Saclay (ComUE), Univ Paris 11, CNRS, Inst Astrophys Spatiale
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  • S. Basu, Yale Univ, Yale University, Dept Astron
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  • T. R. Bedding, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys
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  • O. Benomar, New York Univ Abu Dhabi, Ctr Space Sci, NYUAD Inst
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  • R. A. Garcia, Univ Paris Diderot, CEA, University of Paris Diderot - Paris VII, Universite Sorbonne Paris Cite-USPC (COMUE), Centre National de la Recherche Scientifique (CNRS), Lab AIM, CEA, DRF,CNRS,IRFU,SAp,Ctr Saclay
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  • D. Huber, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys
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  • Hans Kjeldsen
  • D. W. Latham, Harvard University
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  • T. S. Metcalfe, Space Telescope Sci Inst
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  • P. I. Papics, Katholieke Univ Leuven, KU Leuven, Inst Sterrenkunde
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  • T. R. White, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys, Australian Natl Univ, Australian National University, Mt Stromlo Observ, Res Sch Astron & Astrophys
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  • C. Aerts, Radboud Univ Nijmegen, Radboud University Nijmegen, IMAPP, Dept Astrophys
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  • J. Ballot, Univ Toulouse, Centre National de la Recherche Scientifique (CNRS), PRES Universite de Toulouse, Universite Toulouse III - Paul Sabatier, Universite de Toulouse, IRAP, UPS OMP
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  • T. S. Boyajian, Yale Univ, Yale University, Dept Astron
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  • M. Briquet, Univ Liege, University of Liege, Inst Astrophys & Geophys, Quartier Agora
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  • H. Bruntt, Aarhus Katedralskole
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  • L. A. Buchhave, University of Copenhagen
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  • T. L. Campante, Univ Birmingham, University of Birmingham, Sch Phys & Astron
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  • G. Catanzaro, INAF Osservatorio Astrofis Catania, Istituto Nazionale Astrofisica - Italy
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  • J. Christensen-Dalsgaard
  • G. R. Davies, Univ Paris Diderot, CEA, University of Paris Diderot - Paris VII, Universite Sorbonne Paris Cite-USPC (COMUE), Centre National de la Recherche Scientifique (CNRS), Lab AIM, CEA, DRF,CNRS,IRFU,SAp,Ctr Saclay
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  • G. Dogan
  • D. Dragomir, Univ Chicago, University of Chicago, Dept Astron & Astrophys
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  • A. P. Doyle, Univ Warwick, University of Warwick, Dept Phys
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  • Y. Elsworth, Univ Birmingham, University of Birmingham, Sch Phys & Astron
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  • A. Frasca, INAF Osservatorio Astrofis Catania, Istituto Nazionale Astrofisica - Italy
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  • P. Gaulme, New Mexico State Univ, New Mexico State University, Dept Astron
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  • M. Gruberbauer, St Marys Univ, Saint Marys University - Canada, Dept Phys & Astron, Inst Computat Astrophys
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  • R. Handberg
  • S. Hekker, Max Planck Inst Solar Syst Res, Max Planck Society, SAGE Res Grp
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  • C. Karoff
  • H. Lehmann, Thuringer Landessternwarte Tautenburg TLS
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  • P. Mathias, Univ Toulouse, Centre National de la Recherche Scientifique (CNRS), PRES Universite de Toulouse, Universite Toulouse III - Paul Sabatier, Universite de Toulouse, IRAP, UPS OMP
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  • S. Mathur, Space Telescope Sci Inst
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  • A. Miglio, Univ Birmingham, University of Birmingham, Sch Phys & Astron
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  • J. Molenda-Zakowicz, Uniwersytetu Wroclawskiego, University of Wroclaw, Inst Astron
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  • B. Mosser, Univ Paris Diderot, Centre National de la Recherche Scientifique (CNRS), University of Paris Diderot - Paris VII, Universite Sorbonne Paris Cite-USPC (COMUE), Pierre & Marie Curie University - Paris 6, PSL Research University Paris, Observatoire de Paris, Univ Paris 06, Sorbonne Paris Cite, LESIA,Observ Paris,CNRS,Sorbonne Univ
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  • S. J. Murphy, Univ Sydney, University of Sydney, Sydney Inst Astron SIfA, Sch Phys
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  • C. Regulo, Univ La Laguna, Universidad de la Laguna, Dept Astron
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  • V. Ripepi, INAF Osservatorio Astron Capodimonte, Istituto Nazionale Astrofisica - Italy
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  • D. Salabert, Univ Paris Diderot, CEA, University of Paris Diderot - Paris VII, Universite Sorbonne Paris Cite-USPC (COMUE), Centre National de la Recherche Scientifique (CNRS), Lab AIM, CEA, DRF,CNRS,IRFU,SAp,Ctr Saclay
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  • S. G. Sousa, Univ Porto, Universidade do Porto, Inst Astrofis & Ciencias Espaco, CAUP
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  • D. Stello
  • K. Uytterhoeven, Univ La Laguna, Universidad de la Laguna, Dept Astron

theta 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 mu Hz, a large frequency separation of 83.9 +/- 0.4 mu Hz, and maximum oscillation amplitude at frequency nu(max) = 1829 +/- 54 mu Hz. We also present analyses of new ground-based spectroscopic observations, which, combined with interferometric angular diameter measurements, give T-eff = 6697 +/- 78 K, radius 1.49 +/- 0.03 Re-circle dot, [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-circle dot and ages of 1.0-1.6 Gyr. theta Cyg's T-eff and log g place it cooler than the red edge of the gamma Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The pulsation models show gamma Dor gravity modes driven by the convective blocking mechanism, with frequencies of 1-3 cycles per day (11 to 33 mu Hz). However, gravity modes were not seen in Kepler data; one signal at 1.776 cycles per day (20.56 mu Hz) may be attributable to a faint, possibly background, binary.

Original languageEnglish
Article number17
JournalThe Astrophysical Journal
Volume831
Issue1
Number of pages22
ISSN0004-637X
DOIs
Publication statusPublished - 1 Nov 2016

    Research areas

  • asteroseismology, stars: fundamental parameters, stars: interiors, stars: solar-type, MAIN-SEQUENCE STARS, GAMMA DORADUS STARS, F-TYPE STARS, EXOPLANET HOST STARS, INFRARED FLUX METHOD, EFFECTIVE TEMPERATURES, NEARBY STARS, DELTA SCT, A-TYPE, SPECTROSCOPIC PARAMETERS

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