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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

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avis › Tidsskriftartikel › Forskning › peer review

DOI

  • 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
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  • W. J. Chaplin, University of Birmingham
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  • B. Smalley, Keele University
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  • D. W. Kurtz, University of Central Lancashire
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  • R. L. Gilliland, Pennsylvania State University
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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, Université Paris-Saclay (Paris XI)
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  • S. Basu, Yale University
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  • T. R. Bedding, University of Sydney
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  • O. Benomar, New York Univ Abu Dhabi, Ctr Space Sci, NYUAD Inst
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  • R. A. Garcia, Université Paris Cité (Paris V, Paris VII)
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  • D. Huber, University of Sydney
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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, KU Leuven
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  • T. R. White, University of Sydney, Australian National University
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  • C. Aerts, Radboud University Nijmegen
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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 University
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  • M. Briquet, University of Liege
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  • H. Bruntt, Aarhus Katedralskole
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  • L. A. Buchhave, Københavns Universitet
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  • T. L. Campante, University of Birmingham
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  • G. Catanzaro, National Institute for Astrophysics
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  • J. Christensen-Dalsgaard
  • G. R. Davies, Université Paris Cité (Paris V, Paris VII)
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  • G. Dogan
  • D. Dragomir, University of Chicago
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  • A. P. Doyle, University of Warwick
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  • Y. Elsworth, University of Birmingham
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  • A. Frasca, National Institute for Astrophysics
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  • P. Gaulme, New Mexico State University
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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 Tautenberg
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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, University of Birmingham
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  • J. Molenda-Zakowicz, University of Wroclaw
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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), PSL Research University Paris, Observatoire de Paris, PSL Res Univ, CNRS, GEPI,Observ Paris,Sorbonne Paris Cite
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  • S. J. Murphy, University of Sydney
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  • C. Regulo, University of La Laguna
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  • V. Ripepi, National Institute for Astrophysics
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  • D. Salabert, Université Paris Cité (Paris V, Paris VII)
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  • S. G. Sousa, University of Porto
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  • D. Stello
  • K. Uytterhoeven, University of La Laguna

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.

OriginalsprogEngelsk
Artikelnummer17
TidsskriftThe Astrophysical Journal
Vol/bind831
Nummer1
Antal sider22
ISSN0004-637X
DOI
StatusUdgivet - 1 nov. 2016

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