Asteroseismic masses of four evolved planet-hosting stars using SONG and TESS: Resolving the retired A-star mass controversy

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  • Sai Prathyusha Malla, University of New South Wales
  • ,
  • Dennis Stello
  • Daniel Huber, University of Hawaii
  • ,
  • Benjamin T. Montet, University of New South Wales
  • ,
  • Timothy R. Bedding, University of Sydney
  • ,
  • Mads Fredslund Andersen
  • Frank Grundahl
  • Jens Jessen-Hansen
  • Daniel R. Hey, University of Sydney
  • ,
  • Pere L. Palle, Instituto Astrofisico de Canarias, University of La Laguna
  • ,
  • Licai Deng, CAS - National Astronomical Observatories
  • ,
  • Chunguang Zhang, Chinese Academy of Sciences
  • ,
  • Xiaodian Chen, CAS - National Astronomical Observatories
  • ,
  • James Lloyd, Cornell University
  • ,
  • Victoria Antoci, DTU –Space

The study of planet occurrence as a function of stellar mass is important for a better understanding of planet formation. Estimating stellar mass, especially in the red giant regime, is difficult. In particular, stellar masses of a sample of evolved planet-hosting stars based on spectroscopy and grid-based modelling have been put to question over the past decade with claims they were overestimated. Although efforts have been made in the past to reconcile this dispute using asteroseismology, results were inconclusive. In an attempt to resolve this controversy, we study four more evolved planet-hosting stars in this paper using asteroseismology, and we revisit previous results to make an informed study of the whole ensemble in a self-consistent way. For the four new stars, we measure their masses by locating their characteristic oscillation frequency, vmax, from their radial velocity time series observed by SONG. For two stars, we are also able to measure the large frequency separation, A v, helped by extended SONG single-site and dual-site observations and new Transiting Exoplanet Survey Satellite observations. We establish the robustness of the vmax-only-based results by determining the stellar mass from Av, and from both Av and vmax. We then compare the seismic masses of the full ensemble of 16 stars with the spectroscopic masses from three different literature sources. We find an offset between the seismic and spectroscopic mass scales that is mass dependent, suggesting that the previously claimed overestimation of spectroscopic masses only affects stars more massive than about 1.6 M.

Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Pages (from-to)5423-5435
Number of pages13
Publication statusPublished - Aug 2020

    Research areas

  • Stars: evolution, Stars: fundamental parameters, Stars: oscillations, Techniques: radial velocities

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ID: 201059964