Sebastian, D, Swayne, MI, Maxted, PFL, Triaud, AHMJ, Sousa, SG, Olofsson, G, Beck, M, Billot, N, Hoyer, S, Gill, S, Heidari, N, Martin, DV, Persson, CM, Standing, MR, Alibert, Y, Alonso, R, Anglada, G, Asquier, J, Bárczy, T, Barrado, D, Barros, SCC, Battley, MP, Baumjohann, W, Beck, T, Benz, W, Bergomi, M, Boisse, I, Bonfils, X, Brandeker, A, Broeg, C, Cabrera, J, Charnoz, S, Cameron, AC, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demangeon, ODS, Demory, B-O, Dransfield, G, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Hasiba, J, Hébrard, G, Heng, K, Isaak, KG, Kiss, LL, Kopp, E, Kunovac, V, Laskar, J, des Etangs, AL, Lendl, M, Lovis, C, Magrin, D, McCormac, J, Miller, NJ, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Pepe, FA, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Lalitha, S, Santerne, A, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Udry, S, Van Grootel, V and Walton, NA (2022) The EBLM project – IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves. Monthly Notices of the Royal Astronomical Society. ISSN 0035-8711

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<jats:title>Abstract</jats:title> <jats:p>Eclipsing binaries are important benchmark objects to test and calibrate stellar structure and evolution models. This is especially true for binaries with a fully convective M-dwarf component for which direct measurements of these stars’ masses and radii are difficult using other techniques. Within the potential of M-dwarfs to be exoplanet host stars, the accuracy of theoretical predictions of their radius and effective temperature as a function of their mass is an active topic of discussion. Not only the parameters of transiting exoplanets but also the success of future atmospheric characterisation rely on accurate theoretical predictions. We present the analysis of five eclipsing binaries with low-mass stellar companions out of a sub-sample of 23, for which we obtained ultra high-precision light curves using the CHEOPS satellite. The observation of their primary and secondary eclipses are combined with spectroscopic measurements to precisely model the primary parameters and derive the M-dwarfs mass, radius, surface gravity, and effective temperature estimates using the PYCHEOPS data analysis software. Combining these results to the same set of parameters derived from TESS light curves, we find very good agreement (better than 1% for radius and better than 0.2% for surface gravity). We also analyse the importance of precise orbits from radial velocity measurements and find them to be crucial to derive M-dwarf radii in a regime below 5% accuracy. These results add five valuable data points to the mass-radius diagram of fully-convective M-dwarfs.</jats:p>

Item Type: Article
Additional Information: © The Author(s) 2022. Published by Oxford University Press on behalf of The Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (, which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
Uncontrolled Keywords: binaries: eclipsing; stars: fundamental parameters; stars: low-mass; techniques: photometric; techniques: spectroscopic
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 28 Sep 2022 12:35
Last Modified: 28 Sep 2022 12:35

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