Spectroscopic confirmation of the binary nature of the hybrid pulsator KIC 5709664 found with the frequency modulation method

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  • A. Derekas, Eötvös Loránd University, Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary, MTA-ELTE Exoplanet Research Group
  • ,
  • S. J. Murphy, Sydney University, Sydney
  • ,
  • G. Dálya, Eötvös Loránd University
  • ,
  • R. Szabó, Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary, Research Institute for Soil Science and Agricultural Chemistry (RISSAC) of the Hungarian Academy of Sciences
  • ,
  • T. Borkovits, Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary, University of Szeged
  • ,
  • A. Bókon, University of Szeged
  • ,
  • H. Lehmann
  • K. Kinemuchi, Apache Point Observatory
  • ,
  • J. Southworth, Keele University
  • ,
  • S. Bloemen, Radboud University Nijmegen
  • ,
  • B. Csák, Eötvös Loránd University, Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary
  • ,
  • H. Isaacson, UC Berkeley
  • ,
  • J. Kovács, Eötvös Loránd University, MTA-ELTE Exoplanet Research Group
  • ,
  • A. Shporer, Massachusetts Institute of Technology
  • ,
  • G. M. Szabó, Eötvös Loránd University, MTA-ELTE Exoplanet Research Group
  • ,
  • A. O. Thygesen, California Institute of Technology
  • ,
  • S. Mészáros, Eötvös Loránd University, MTA-ELTE Exoplanet Research Group

We started a program to search for companions around hybrid δ Sct/γ Dor stars with the frequency modulation method using Kepler data. Our best candidate was KIC 5709664, where we could identify Fourier peaks with sidelobes, suggesting binary orbital motion. We determined the orbital parameters with the phase modulation method and took spectroscopic measurements to confirm unambiguously the binary nature with radial velocities. The spectra show that the object is a double-lined spectroscopic binary, and we determined the orbital solutions from the radial velocity curve fit. The parameters from the phase modulation method and the radial velocity fits are in good agreement. We combined a radial velocity and phase modulation approach to determine the orbital parameters as accurately as possible. We determined that the pulsator is a hybrid δ Sct/γ Dor star in an eccentric binary system with an orbital period of ∼95 d and an eccentricity of 0.55. The measured mass ratio is 0.67. We analysed the pulsation content and extracted 38 frequencies with amplitudes greater than 20 μmag. At low frequencies, we found broad power excesses which are likely attributed to spots on the rotating surface of the lower mass component. We inferred rotation periods of 0.56 and 2.53 d for the primary and secondary, respectively.

OriginalsprogEngelsk
TidsskriftMonthly Notices of the Royal Astronomical Society
Vol/bind486
Nummer2
Sider (fra-til)2129-2136
Antal sider8
ISSN0035-8711
DOI
StatusUdgivet - jun. 2019

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