Volume 622, February 2019
|Number of page(s)||12|
|Section||Stellar structure and evolution|
|Published online||18 February 2019|
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Ny Munkegade, 8000 Aarhus C., Denmark
2 Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China
3 Department of Astronomy, China West Normal University, Nanchong 637002, PR China
4 Center for Cosmology and Particle Physics, Dept. of Physics, New York University, 726 Broadway, New York, NY 10003, USA
5 Institute for Astronomy, University of Hawai‘i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
6 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia
7 Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
8 Universidad de La Laguna, Dpto. Astrofísica, 38206 La Laguna, Tenerife, Spain
9 IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France
10 Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, 91191 Gif-sur-Yvette, France
11 School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia
12 Centre for Star and Planet Formation, Niels Bohr Institute, University of Copenhagen, Øster Voldgade 5, 1350 Copenhagen, Denmark
Accepted: 4 January 2019
Context. Asteroseismic analysis of solar-like stars allows us to determine physical parameters such as stellar mass, with a higher precision compared to most other methods. Even in a well-studied cluster such as the Hyades, the masses of the red giant stars are not well known, and previous mass estimates are based on model calculations (isochrones). The four known red giants in the Hyades are assumed to be clump (core-helium-burning) stars based on their positions in colour-magnitude diagrams, however asteroseismology offers an opportunity to test this assumption.
Aims. Using asteroseismic techniques combined with other methods, we aim to derive physical parameters and the evolutionary stage for the planet hosting star ϵ Tau, which is one of the four red giants located in the Hyades.
Methods. We analysed time-series data from both ground and space to perform the asteroseismic analysis. By combining high signal-to-noise radial-velocity data from the ground-based SONG network with continuous space-based data from the revised Kepler mission K2, we derive and characterize 27 individual oscillation modes for ϵ Tau, along with global oscillation parameters such as the large frequency separation Δν and the ratio between the amplitude of the oscillations measured in radial velocity and intensity as a function of frequency. The latter has been measured previously for only two stars, the Sun and Procyon. Combining the seismic analysis with interferometric and spectroscopic measurements, we derive physical parameters for ϵ Tau, and discuss its evolutionary status.
Results. Along with other physical parameters, we derive an asteroseismic mass for ϵ Tau of M = 2.458 ± 0.073 M⊙, which is slightly lower than previous estimates, and which leads to a revised minimum mass of the planetary companion. Noting that the SONG and K2 data are non-simultaneous, we estimate the amplitude ratio between intensity and radial velocity to be 42.2 ± 2.3 ppm m−1 s, which is higher than expected from scaling relations.
Key words: asteroseismology / techniques: radial velocities / techniques: photometric / stars: individual: HD 28305 / stars: oscillations / planetary systems
Time-series data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/622/A190
Based on observations made with the SONG telescopes operated on the Spanish Observatorio del Teide (Tenerife) and at the Chinese Delingha Observatory (Qinghai) by the Aarhus and Copenhagen Universities, by the Instituto de Astrofísica de Canarias and by the National Astronomical Observatories of China, and with NASA’s K2 mission.
© ESO 2019
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