Precision Orbit of δ Delphini and Prospects for Astrometric Detection of Exoplanets

Combining visual and spectroscopic orbits of binary stars leads to a determination of the full 3D orbit, individual masses, and distance to the system. We present a full analysis of the evolved binary system δ Delphini using astrometric data from the MIRC and PAVO instruments on the CHARA long-basel...

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Bibliographic Details
Published in:The Astrophysical journal 2018-03, Vol.855 (1), p.1
Main Authors: Gardner, Tyler, Monnier, John D., Fekel, Francis C., Williamson, Mike, Duncan, Douglas K., White, Timothy R., Ireland, Michael, Adams, Fred C., Barman, Travis, Baron, Fabien, Brummelaar, Theo ten, Che, Xiao, Huber, Daniel, Kraus, Stefan, Roettenbacher, Rachael M., Schaefer, Gail, Sturmann, Judit, Sturmann, Laszlo, Swihart, Samuel J., Zhao, Ming
Format: Article
Language:English
Subjects:
Astrometry
Astronomical models
Astrophysics
binaries: close
binaries: spectroscopic
binaries: visual
Binary stars
Companion stars
Detection limits
Extrasolar planets
Interferometers
Mass transfer
Observatories
Orbital elements
Orbits
Personal computers
Planet detection
Planetary evolution
Planetary orbits
planets and satellites: detection
Stellar age
Stellar evolution
Stellar models
Stellar system evolution
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Summary:Combining visual and spectroscopic orbits of binary stars leads to a determination of the full 3D orbit, individual masses, and distance to the system. We present a full analysis of the evolved binary system δ Delphini using astrometric data from the MIRC and PAVO instruments on the CHARA long-baseline interferometer, 97 new spectra from the Fairborn Observatory, and 87 unpublished spectra from the Lick Observatory. We determine the full set of orbital elements for δ Del, along with masses of 1.78 0.07 M and 1.62 0.07 M for each component, and a distance of 63.61 0.89 pc. These results are important in two contexts: for testing stellar evolution models and for defining the detection capabilities for future planet searches. We find that the evolutionary state of this system is puzzling, as our measured flux ratios, radii, and masses imply a ∼200 Myr age difference between the components, using standard stellar evolution models. Possible explanations for this age discrepancy include mass transfer scenarios with a now-ejected tertiary companion. For individual measurements taken over a span of two years, we achieve 2 MJ on orbits >0.75 au around individual components of hot binary stars via differential astrometry.
ISSN:0004-637X
1538-4357
1538-4357
DOI:10.3847/1538-4357/aaac80