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  The TESS light curve of AI Phoenicis

Maxted, P. F. L., Gaulme, P., Graczyk, D., Hełminiak, K. G., Johnston, C., Orosz, J. A., et al. (2020). The TESS light curve of AI Phoenicis. Monthly Notices of the Royal Astronomical Society, 498(1). doi:10.1093/mnras/staa1662.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0007-0AD6-D Version Permalink: http://hdl.handle.net/21.11116/0000-0007-0AD7-C
Genre: Journal Article

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 Creators:
Maxted, P F L, Author
Gaulme, Patrick1, Author              
Graczyk, D, Author
Hełminiak, K G, Author
Johnston, C, Author
Orosz, Jerome A, Author
Prša, Andrej, Author
Southworth, John, Author
Torres, Guillermo, Author
Davies, Guy R, Author
Ball, Warrick, Author
Chaplin, William J, Author
Affiliations:
1Department Solar and Stellar Interiors, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832287              

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Free keywords: stars: solar-type, stars: fundamental parameters, binaries: eclipsing, stars: individual: AI Phe
 Abstract: Accurate masses and radii for normal stars derived from observations of detached eclipsing binary stars are of fundamental importance for testing stellar models and may be useful for calibrating free parameters in these model if the masses and radii are sufficiently precise and accurate. We aim to measure precise masses and radii for the stars in the bright eclipsing binary AI Phe, and to quantify the level of systematic error in these estimates. We use several different methods to model the TESS light curve of AI Phe combined with spectroscopic orbits from multiple sources to estimate precisely the stellar masses and radii together with robust error estimates. We find that the agreement between different methods for the light curve analysis is very good but some methods underestimate the errors on the model parameters. The semi-amplitudes of the spectroscopic orbits derived from spectra obtained with modern échelle spectrographs are consistent to within 0.1%. The masses of the stars in AI Phe are M1=1.1938±0.0008M and M2=1.2438±0.0008M , and the radii are R1=1.8050±0.0022R and R2=2.9332±0.0023R . We conclude that it is possible to measure accurate masses and radii for stars in bright eclipsing binary stars to a precision of 0.2% or better using photometry from TESS and spectroscopy obtained with modern échelle spectrographs. We provide recommendations for publishing masses and radii of eclipsing binary stars at this level of precision.

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Language(s): eng - English
 Dates: 2020
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa1662
ADS: 2020MNRAS.tmp.1795M
arXiv: 2003.09295
 Degree: -

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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Affiliations:
Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 498 (1) Sequence Number: - Start / End Page: - Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150