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Mikkel Nørup Lund

Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65

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  • W. J. Chaplin, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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  • R. Sanchis-Ojeda, Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
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  • T. L. Campante, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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  • R. Handberg
  • D. Stello, Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, Australia
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  • J. N. Winn, Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
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  • S. Basu, Department and Astronomy, Yale University, New Haven, CT 06520, USA
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  • J. Christensen-Dalsgaard
  • G. R. Davies, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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  • T. S. Metcalfe, White Dwarf Research Corporation, Boulder, CO 80301, USA
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  • L. A. Buchhave, Københavns Universitet
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  • D. A. Fischer, Department and Astronomy, Yale University, New Haven, CT 06520, USA
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  • T. R. Bedding, Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, Australia
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  • W. D. Cochran, McDonald Observatory, The University of Texas, Austin, TX 78712, USA
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  • Y. Elsworth, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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  • R. L. Gilliland, Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, University Park, PA 16802, USA
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  • S. Hekker, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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  • D. Huber, NASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USA
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  • H. Isaacson, Department of Astronomy, University of California, Berkeley, CA 94720, USA
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  • C. Karoff
  • S. D. Kawaler, Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA
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  • H. Kjeldsen
  • D. W. Latham, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
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  • M. N. Lund
  • M. Lundkvist
  • G. W. Marcy, Department of Astronomy, University of California, Berkeley, CA 94720, USA
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  • A. Miglio, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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  • T. Barclay, NASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USA
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  • J. J. Lissauer, NASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USA
Results on the obliquity of exoplanet host stars—the angle between the stellar spin axis and the planetary orbital axis—provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1σ level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favored in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated.
OriginalsprogEngelsk
TidsskriftAstrophysical Journal
Vol/bind766
Sider (fra-til)101
ISSN0004-637X
DOI
StatusUdgivet - 1 apr. 2013

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