Parameters of the eclipsing binary α Draconis observed by TESS and SONG
Article
Article Title | Parameters of the eclipsing binary α Draconis observed by TESS and SONG |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Hey, Daniel R. (Author), Kochoska, Angela (Author), Monier, Richard (Author), Kochukhov, Oleg (Author), Johnston, Cole (Author), Bedding, Timothy R. (Author), Murphy, Simon J. (Author), Abdul-Masih, Michael (Author), Southworth, John (Author), Andersen, Mads Fredslund (Author), Grundahl, Frank (Author) and Palle, Pere L. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 511 (2), pp. 2648-2658 |
Number of Pages | 11 |
Year | 2022 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stac020 |
Web Address (URL) | https://academic.oup.com/mnras/article/511/2/2648/6507583 |
Abstract | We present an analysis of the eclipsing single-lined spectroscopic binary system α Dra based on photometry from the Transiting Exoplanet Survey Satellite (TESS) mission and newly acquired spectroscopic measurements. Recently discovered to have eclipses in the TESS data, at a magnitude of V = 3.7, α Dra is now one of the brightest detached eclipsing binary (EB) systems known. We obtain the parameters of this system by simultaneously fitting the TESS light curve in conjunction with radial velocities (RVs) acquired from the SONG spectrograph. We determine the fractional radii (R/a) for the primary and secondary components of the system to be 0.0479 ± 0.0003 and 0.0226 ± 0.0005, respectively. We constrain the temperature, mass, and luminosity (log(L/L⊙)) of the primary to be 9975±125 K, 3.7±0.1 M⊙, and 2.49±0.02, respectively, using isochrone fitting. Although the secondary is too faint to appear in the spectra, the obtained mass function and observed inclination yields a secondary minimum mass of M2=2.5±0.1 M⊙, which suggests that it is an A2V type star. We were unable to obtain RVs of the secondary, and are only able to see a weak highly rotationally broadened absorption line, indicating that the secondary is rapidly rotating (vsin i ∼ 200 km s−1). We also perform an abundance analysis of the primary star for 21 chemical elements. We find a complex abundance pattern, with a few elements having mild underabundances while the majority have solar abundances. We make available the PYTHON code used in this paper to facilitate future modelling of EBs. |
Keywords | binaries: eclipsing; stars: chemically peculiar; stars: fundamental parameters |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2022 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | University of Sydney |
Villanova University, United States | |
Sorbonne University, France | |
Uppsala University, Sweden | |
Catholic University of Leuven, Belgium | |
European Southern Observatory (ESO), Chile | |
Keele University, United Kingdom | |
Aarhus University, Denmark | |
Institute of Astrophysics of the Canary Islands, Spain | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q7387/parameters-of-the-eclipsing-binary-draconis-observed-by-tess-and-song
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