Fulltext

Disentangling stellar activity and planetary signals

Boisse, Isabelle ; Bouchy, François ; Hébrard, Guillaume ; Bonfils, Xavier ; Santos, Nuno ; Vauclair, Sylvie

In: Proceedings of the International Astronomical Union, 2010, vol. 6, no. S276, p. 399-400

Aggiungi alla tua lista
    Titre
    • Disentangling stellar activity and planetary signals
    Auteur
    • Boisse, Isabelle. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, UMR7095 CNRS, 98bis bd. Arago, 75014 Paris, France, email: iboisse@iap.fr
    • Bouchy, François. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, UMR7095 CNRS, 98bis bd. Arago, 75014 Paris, France, email: iboisse@iap.fr
    • Hébrard, Guillaume. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, UMR7095 CNRS, 98bis bd. Arago, 75014 Paris, France, email: iboisse@iap.fr
    • Bonfils, Xavier. Laboratoire d'Astrophysique de Grenoble, Observatoire de Grenoble, Université Joseph Fourier, CNRS, UMR 5571, 38041, Grenoble Cedex 09, France
    • Santos, Nuno. Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
    • Vauclair, Sylvie. LATT-UMR 5572, CNRS & Université P. Sabatier, 14 Av. E. Belin, 31400 Toulouse, France
    Type de document
    • Postprint
    Langue
    • Inglese
    Publié dans
    • Proceedings of the International Astronomical Union, 2010, vol. 6, no. S276, p. 399-400. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:304806
    Summary
    High-precision radial-velocimetry (RV) is until now the more efficient way to discover planetary systems. Moreover, photometric transit search missions like CoRoT and Kepler, need spectroscopic RV measurements to establish the planetary nature of a transit candidate and to measure the true mass. An active star has on its photosphere dark spots and bright plages rotating with the star. These inhomogeneities of the stellar surface can induce a variation of the measurement of the RV, due to changes in lines shapes and not to a Doppler motion of the star (e.g. Queloz et al. 2001; Desort et al. 2007; Boisse et al. 2009). We study how the Keplerian fit used to search for planets in RV data is confused by spots and we test an approach to subtract RV jitter based on harmonic decomposition of the star rotation. We use simulations of spectroscopic measurements of rotating spotted stars and validate our approach on active stars monitored by high-precision spectrograph HARPS: CoRoT-7 and ι Hor