A simple model to describe intrinsic stellar noise for exoplanet detection around red giants

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DOI

    Thomas S. H. North, Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark txn016@bham.ac.uk, William J. Chaplin, Ronald L. Gilliland, Space Telescope Science Institute, Science Mission Office, 3700 San Martin Drive, Baltimore, MD 21218, USA, Daniel Huber, Tiago L. Campante,
  • Rasmus Handberg
  • Mikkel N. Lund
  • Dimitri Veras, Department of Physics, University of Warwick, Coventry CV4 7AL, UK, James S. Kuszlewicz, Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark, Will M. Farr, School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
In spite of the huge advances in exoplanet research provided by the NASA Kepler Mission, there remain only a small number of transit detections around evolved stars. Here, we present a reformulation of the noise properties of red-giant stars, where the intrinsic stellar granulation and the stellar oscillations described by asteroseismology play a key role. The new noise model is a significant improvement on the current Kepler results for evolved stars. Our noise model may be used to help understand planet detection thresholds for the ongoing K2 and upcoming TESSmissions, and serve as a predictor of stellar noise for these missions. As an application of our noise model, we explore the minimum detectable planet radii for red giant stars, and find that Neptune-sized planets should be detectable around low-luminosity red giant branch stars.
Original languageEnglish
JournalRoyal Astronomical Society. Monthly Notices
Volume465
Issue number2
Pages (from-to)1308-1315
ISSN0035-8711
DOIs
StatePublished - 1 Feb 2017

    Research areas

  • asteroseismology, techniques: photometric, planetary systems

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