Robust asteroseismic properties of the bright planet host HD 38529

Warrick H. Ball, William J. Chaplin, Martin B. Nielsen, Lucia González-Cuesta, Savita Mathur, Ângela R. G. Santos, Rafael García, Derek Buzasi, Benoît Mosser, Morgan Deal, Amalie Stokholm, Jakob Rørsted Mosumgaard, Victor Silva Aguirre, Benard Nsamba, Tiago Campante, Margarida S. Cunha, Joel Ong, Sarbani Basu, Sibel Örtel, Z. Çelik OrhanMutlu Yıldız, Keivan Stassun, Stephen R. Kane, Daniel Huber

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The Transiting Exoplanet Survey Satellite (TESS) is recording short-cadence, high duty-cycle timeseries across most of the sky, which presents the opportunity to detect and study oscillations in interesting stars, in particular planet hosts. We have detected and analysed solar-like oscillations in the bright G4 subgiant HD 38529, which hosts an inner, roughly Jupiter-mass planet on a 14.3d orbit and an outer, low-mass brown dwarf on a 2136d orbit. We combine results from multiple stellar modelling teams to produce robust asteroseismic estimates of the star’s properties, including its mass M=1.48±0.04M⊙⁠, radius R=2.68±0.03R⊙⁠, and age t=3.07±0.39Gyr⁠. Our results confirm that HD 38529 has a mass near the higher end of the range that can be found in the literature and also demonstrate that precise stellar properties can be measured given shorter timeseries than produced by CoRoT, Kepler, or K2.
Original languageEnglish
Pages (from-to)6084–6093
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
Early online date17 Oct 2020
Publication statusPublished - Dec 2020

Bibliographical note

10 pages, 6 figures, 4 tables, accepted for publication in MNRAS


  • stars: oscillations
  • stars: individual (HD 38529)


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