Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obtained new radial velocities from echelle spectra using the APO 3.5 m, CTIO 1.5 m, and Fairborn Observatory 2.0 m telescop...
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| Published in | The Astronomical journal Vol. 164; no. 6; pp. 228 - 247 |
|---|---|
| Main Authors | , , , , , , , , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Madison
The American Astronomical Society
01.12.2022
IOP Publishing American Astronomical Society |
| Subjects | |
| Online Access | Get full text |
| ISSN | 0004-6256 1538-3881 1538-3881 |
| DOI | 10.3847/1538-3881/ac9385 |
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| Abstract | We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obtained new radial velocities from echelle spectra using the APO 3.5 m, CTIO 1.5 m, and Fairborn Observatory 2.0 m telescopes. By combining the astrometric and spectroscopic observations, we solve for the full, three-dimensional orbits and determine the stellar masses to 1%–12% uncertainty and distances to 0.4%–6% uncertainty. We then estimate the effective temperature and radius of each component star through Doppler tomography and spectral energy distribution analyses. We found masses of 1.4–3.5
M
⊙
, radii of 1.5–4.7
R
⊙
, and temperatures of 6400–10,300 K. We then compare the observed stellar parameters to the predictions of the stellar evolution models, but found that only one of our systems fits well with the evolutionary models. |
|---|---|
| AbstractList | We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obtained new radial velocities from echelle spectra using the APO 3.5 m, CTIO 1.5 m, and Fairborn Observatory 2.0 m telescopes. By combining the astrometric and spectroscopic observations, we solve for the full, three-dimensional orbits and determine the stellar masses to 1%–12% uncertainty and distances to 0.4%–6% uncertainty. We then estimate the effective temperature and radius of each component star through Doppler tomography and spectral energy distribution analyses. We found masses of 1.4–3.5 M⊙, radii of 1.5–4.7 R⊙, and temperatures of 6400–10,300 K. We then compare the observed stellar parameters to the predictions of the stellar evolution models, but found that only one of our systems fits well with the evolutionary models. We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obtained new radial velocities from echelle spectra using the APO 3.5 m, CTIO 1.5 m, and Fairborn Observatory 2.0 m telescopes. By combining the astrometric and spectroscopic observations, we solve for the full, three-dimensional orbits and determine the stellar masses to 1%-12% uncertainty and distances to 0.4%-6% uncertainty. We then estimate the effective temperature and radius of each component star through Doppler tomography and spectral energy distribution analyses. We found masses of 1.4-3.5 M ⊙, radii of 1.5-4.7 R ⊙, and temperatures of 6400-10,300 K. We then compare the observed stellar parameters to the predictions of the stellar evolution models, but found that only one of our systems fits well with the evolutionary models. We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obtained new radial velocities from echelle spectra using the APO 3.5 m, CTIO 1.5 m, and Fairborn Observatory 2.0 m telescopes. By combining the astrometric and spectroscopic observations, we solve for the full, three-dimensional orbits and determine the stellar masses to 1%–12% uncertainty and distances to 0.4%–6% uncertainty. We then estimate the effective temperature and radius of each component star through Doppler tomography and spectral energy distribution analyses. We found masses of 1.4–3.5 M ⊙ , radii of 1.5–4.7 R ⊙ , and temperatures of 6400–10,300 K. We then compare the observed stellar parameters to the predictions of the stellar evolution models, but found that only one of our systems fits well with the evolutionary models. |
| Author | Chojnowski, S. Drew Gies, Douglas R. Setterholm, Benjamin R. Gardner, Tyler Monnier, John D. Labdon, Aaron Fekel, Francis C. Davies, Claire L. Schaefer, Gail H. Anugu, Narsireddy Hubbard-James, Hodari-Sadiki Bouquin, Jean-Baptiste Le Lanthermann, Cyprien Lester, Kathryn V. Jao, Wei-Chun Brummelaar, Theo Ten Farrington, Christopher D. Gordon, Kathryn D. Paredes, Leonardo A. Henry, Todd J. Kraus, Stefan |
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| Keywords | Long baseline interferometry Fundamental parameters of stars Visual binary stars Binary stars Spectroscopic binary stars Astrophysics - Solar and Stellar Astrophysics |
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| Snippet | We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the... |
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| SubjectTerms | Arrays Astronomical models Astronomy Astrophysics Binary stars Fundamental parameters of stars Interferometry Long baseline interferometry Orbits Sciences of the Universe Spectral energy distribution Spectroscopic binary stars Spectroscopic observation Spectroscopic telescopes Spectroscopy Stellar evolution Stellar models Telescopes Uncertainty Visual binary stars |
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| Title | Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692 |
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