000005287 001__ 5287
000005287 005__ 20211221140912.0
000005287 0247_ $$2DOI$$a10.1051/0004-6361/202039389
000005287 037__ $$aSCART-2021-0067
000005287 100__ $$aLampens, P.
000005287 245__ $$aOrbital solutions derived from radial velocities and time delays for four Kepler systems with A/F-type (candidate) hybrid pulsators 
000005287 260__ $$c2021
000005287 520__ $$aThe presence of A/F-type Kepler hybrid stars extending across the entire δ Sct-γ Dor instability strips and beyond remains largely unexplained. In order to better understand these particular stars, we performed a multi-epoch spectroscopic study of 49 candidate A/F-type hybrid stars and one cool(er) hybrid object detected by the Kepler mission. We determined a lower limit of 27% for the multiplicity fraction. For six spectroscopic systems, we also reported long-term variations of the time delays. For four systems, the time delay variations are fully coherent with those of the radial velocities and can be attributed to orbital motion. We aim to improve the orbital solutions for those systems with long orbital periods (order of 4-6 years) among the Kepler hybrid stars. The orbits are computed based on a simultaneous modelling of the RVs obtained with high-resolution spectrographs and the photometric time delays derived from time-dependent frequency analyses of the Kepler light curves. We refined the orbital solutions of four spectroscopic systems with A/F-type Kepler hybrid component stars: KIC4480321, KIC5219533, KIC8975515 and KIC9775454. Simultaneous modelling of both data types analysed together enabled us to improve the orbital solutions, obtain more robust and accurate information on the mass ratio, and identify the component with the short-period δ Sct-type pulsations. In several cases, we were also able to derive new constraints for the minimum component masses. From a search for regular frequency patterns in the high-frequency regime of the Fourier transforms of each system, we found no evidence of tidal splitting among the triple systems with close (inner) companions. However, some systems exhibit frequency spacings which can be explained by the mechanism of rotational splitting.
000005287 594__ $$aNO
000005287 6531_ $$aBinaries: spectroscopic
000005287 6531_ $$aStars: variables: delta Scuti
000005287 6531_ $$aAsteroseismology
000005287 6531_ $$aTechniques: radial velocities
000005287 6531_ $$aTechniques: photometric
000005287 700__ $$aVermeylen, L.
000005287 700__ $$aFrémat, Y.
000005287 700__ $$aSódor, Á.
000005287 700__ $$aSkarka, M.
000005287 700__ $$aSamadi-Ghadim, A.
000005287 700__ $$aBognár, Zs.
000005287 700__ $$aLehmann, H.
000005287 700__ $$aDe Cat, P.
000005287 700__ $$aGoswami, A.
000005287 700__ $$aDumortier, L.
000005287 773__ $$cA139, 1-10$$pAstronomy & Astrophysics$$v647
000005287 8560_ $$fpeter.decat@observatoire.be
000005287 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2021arXiv210106174L/abstract
000005287 8564_ $$s1105225$$uhttp://publi2-as.oma.be/record/5287/files/Lampens2021_AA647_A139.pdf
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000005287 905__ $$apublished in
000005287 980__ $$aREFERD