Seismic constraints on rotation of Sun-like star and mass of exoplanet

Research output: Contribution to journalArticle

Authors

  • Laurent Gizon
  • Jérome Ballot
  • Eric Michel
  • Thorsten Stahn
  • Gérard Vauclair
  • Hans Bruntt
  • Pierre Olivier Quirion
  • Othman Benomar
  • Sylvie Vauclair
  • Thierry Appourchaux
  • Michel Auvergne
  • Annie Baglin
  • Caroline Barban
  • Fréderic Baudin
  • Michaël Bazot
  • Claude Catala
  • Orlagh Creevey
  • Sébastien Deheuvels
  • Noël Dolez
  • Rafael García
  • Patrick Gaulme
  • Stéphane Mathis
  • Savita Mathur
  • Benoît Mosser
  • Clara Régulo
  • Ian Roxburgh
  • David Salabert
  • Réza Samadi
  • Kumiko Sato
  • Shravan Hanasoge
  • Katepalli R. Sreenivasan

Colleges, School and Institutes

External organisations

  • Aarhus Universitet
  • University of Sydney, Austria;
  • Dpto. de Astrofisica, Universidad de La Laguna, La Laguna, 38206, Tenerife, Spain
  • Universidade do Porto
  • Queen Mary University of London
  • PRINCETON UNIVERSITY
  • TUBS, Braunschweig, D-38106, and Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany); AH(School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China
  • Max-Planck-Institut für Astrophysik
  • Georg-August Universität, Institut für Astrophysik, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany
  • Institut de Recherche en Astrophysique et Planétologie
  • Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS, 31400 Toulouse, France
  • Université Pierre et Marie Curie
  • Sydney Institute for Astronomy (SIfA)
  • Institut d'Astrophysique Spatiale (IAS)
  • LAL, Université Paris-Sud, IN2P3/CNRS, F-91898 Orsay, France
  • Centro de Astrofísica and Faculdade de Ciências
  • Astronomy and Physics Department, Saint Mary's University
  • Aarhus University
  • Instituto de Astrofísica de Canarias, E-38200 La Laguna, Spain ; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Spain
  • Dpto de Astrofísica, Universidad de La Laguna, 38206, Tenerife, Spain ; Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
  • Université de Nice Sophia-Antipolis
  • LESIA, UMR8109, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195 Meudon Cedex, France
  • Department of Astronomy
  • High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307, USA
  • National Center for Atmospheric Research
  • Astronomy Unit, Queen Mary, University of London, Mile End Road, London, E1 4NS, UK
  • Department of Geosciences
  • Department of Applied Physics
  • New York University, New York, NY, USA.
  • Centre National de la Recherche Scientifique
  • Université Paul Sabatier
  • Observatoire Midi-Pyrénées
  • Laboratoire D'Études Spatiales et D'Instrumentation en Astrophysique
  • Agence Spatiale Canadienne
  • University of Sydney
  • Universidad de la Laguna
  • Unité Mixte de Recherche 7293
  • Institut de Recherche sur les Lois Fondamentales de L'Univers
  • New Mexico State University Las Cruces
  • Princeton University
  • Courant Institute of Mathematical Sciences

Abstract

Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1:85+0:52 -0:42MJupiter, which implies that it is a planet, not a brown dwarf.

Details

Original languageEnglish
Pages (from-to)13267-13271
Number of pages5
JournalNational Academy of Sciences. Proceedings
Volume110
Issue number33
Publication statusPublished - 13 Aug 2013

Keywords

  • Extrasolar planets, Stellar oscillations, Stellar rotation

ASJC Scopus subject areas