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The excitation of solar-like oscillations in a δ Sct star by efficient envelope convection

Author

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  • V. Antoci

    (Institute of Astronomy, University of Vienna, Türkenschanzstraβe 18, A-1180 Vienna, Austria)

  • G. Handler

    (Institute of Astronomy, University of Vienna, Türkenschanzstraβe 18, A-1180 Vienna, Austria
    Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland)

  • T. L. Campante

    (Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
    Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark)

  • A. O. Thygesen

    (Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
    Nordic Optical Telescope, Apartado 474, E-38700 Santa Cruz de La Palma, Santa Cruz de Tenerife, Spain)

  • A. Moya

    (Centro de Astrobiología, Instituto Nacional de Técnica Aeroespacial – Consejo Superior de Investigaciones Científicas, PO Box 78, E-28691, Villanueva de la Cañada, Madrid, Spain)

  • T. Kallinger

    (Institute of Astronomy, University of Vienna, Türkenschanzstraβe 18, A-1180 Vienna, Austria
    University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada
    Instituut voor Sterrenkunde, University of Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium)

  • D. Stello

    (Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, New South Wales 2006, Australia)

  • A. Grigahcène

    (Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal)

  • H. Kjeldsen

    (Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark)

  • T. R. Bedding

    (Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, New South Wales 2006, Australia)

  • T. Lüftinger

    (Institute of Astronomy, University of Vienna, Türkenschanzstraβe 18, A-1180 Vienna, Austria)

  • J. Christensen-Dalsgaard

    (Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark)

  • G. Catanzaro

    (Istituto Nazionale di Astrofisica – Osservatorio Astrofisico di Catania, via S. Sofia 78, I-95123 Catania, Italy)

  • A. Frasca

    (Istituto Nazionale di Astrofisica – Osservatorio Astrofisico di Catania, via S. Sofia 78, I-95123 Catania, Italy)

  • P. De Cat

    (Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium)

  • K. Uytterhoeven

    (Laboratoire AIM, CEA/DSM-CNRS Université Paris Diderot, Commissariat à l’Energie Atomique et aux Energies Alternatives, Institut de Recherche sur Les Lois Fondamentales, Service d’Astrophysique, Centre de Saclay, F-91191, Gif-sur-Yvette, France
    Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany
    Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
    Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain)

  • H. Bruntt

    (Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark)

  • G. Houdek

    (Institute of Astronomy, University of Vienna, Türkenschanzstraβe 18, A-1180 Vienna, Austria)

  • D. W. Kurtz

    (Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK)

  • P. Lenz

    (Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland)

  • A. Kaiser

    (Institute of Astronomy, University of Vienna, Türkenschanzstraβe 18, A-1180 Vienna, Austria)

  • J. Van Cleve

    (SETI Institute/NASA Ames Research Center, Moffett Field, California 94035, USA)

  • C. Allen

    (Orbital Sciences Corporation/NASA Ames Research Center, Moffett Field, California 94035, USA)

  • B. D. Clarke

    (SETI Institute/NASA Ames Research Center, Moffett Field, California 94035, USA)

Abstract

Delta Scuti (δ Sct)1 stars are opacity-driven pulsators with masses of 1.5–2.5M⊙, their pulsations resulting from the varying ionization of helium. In less massive stars2 such as the Sun, convection transports mass and energy through the outer 30 per cent of the star and excites a rich spectrum of resonant acoustic modes. Based on the solar example, with no firm theoretical basis, models predict that the convective envelope in δ Sct stars extends only about 1 per cent of the radius3, but with sufficient energy to excite solar-like oscillations4,5. This was not observed before the Kepler mission6, so the presence of a convective envelope in the models has been questioned. Here we report the detection of solar-like oscillations in the δ Sct star HD 187547, implying that surface convection operates efficiently in stars about twice as massive as the Sun, as the ad hoc models predicted.

Suggested Citation

  • V. Antoci & G. Handler & T. L. Campante & A. O. Thygesen & A. Moya & T. Kallinger & D. Stello & A. Grigahcène & H. Kjeldsen & T. R. Bedding & T. Lüftinger & J. Christensen-Dalsgaard & G. Catanzaro & A, 2011. "The excitation of solar-like oscillations in a δ Sct star by efficient envelope convection," Nature, Nature, vol. 477(7366), pages 570-573, September.
    • Handle: RePEc:nat:nature:v:477:y:2011:i:7366:d:10.1038_nature10389
    DOI: 10.1038/nature10389
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