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Mikkel Nørup Lund

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 AstronomyAarhus University, Ny Munkegade 120, 8000, Aarhus C, Denmark
  • ,
  • 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 AstronomyAarhus University, Ny Munkegade 120, 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.
OriginalsprogEngelsk
TidsskriftRoyal Astronomical Society. Monthly Notices
Vol/bind465
Nummer2
Sider (fra-til)1308-1315
ISSN0035-8711
DOI
StatusUdgivet - 1 feb. 2017

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