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Published January 1, 2020 | Version v1
Journal article Open

Robust asteroseismic properties of the bright planet host HD 38529

Creators

  • 1. Space Sci Inst, 4765 Walnut St,Suite B, Boulder, CO 80301 USA
  • 2. Florida Gulf Coast Univ, Dept Chem & Phys, 10501 FGCU Blvd, Ft Myers, FL 33965 USA
  • 3. Sorbonne Univ, Univ PSL, Univ Paris, Observ Paris,LESIA,CNRS, F-92195 Meudon, France
  • 4. Univ Porto, Inst Astrofis & Ciencias Espaco, Rua Estrelas, PT-4150762 Porto, Portugal
  • 5. Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
  • 6. Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA
  • 7. Ege Univ, Sci Fac, Dept Astron & Space Sci, TR-35100 Izmir, Turkey

Description

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 2136 d orbit. We combine results frommultiple stellarmodelling teams to produce robust asteroseismic estimates of the star's properties, including its mass M = 1.48 +/- 0.04 M-circle dot, radius R = 2.68 +/- 0.03 R-circle dot, and age t = 3.07 +/- 0.39 Gyr. 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.

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