| Issue |
A&A
Volume 677, September 2023
|
|
|---|---|---|
| Article Number | A154 | |
| Number of page(s) | 11 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202347226 | |
| Published online | 21 September 2023 | |
TIC 43152097 The first eclipsing binary in NGC 2232⋆
1
INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy
e-mail: antonio.frasca@inaf.it
2
INAF – Osservatorio di Astrofisica e Scienza dello Spazio, Via P. Gobetti 93/3, 40129 Bologna, Italy
3
Department of Physics, University of Rome Tor Vergata, Via della Ricerca Scientifica 1, 00133 Rome, Italy
4
INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
5
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, PR China
6
Fundación Galileo Galilei–INAF, Rambla José Ana Fernández Pérez 7, 38712 Breña Baja, Tenerife, Spain
7
INAF – Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monte Porzio Catone, Italy
Received:
19
June
2023
Accepted:
26
July
2023
We report the discovery of a low-mass totally eclipsing system in the young (age ≃ 28 Myr) open cluster NGC 2232, during an examination of their TESS photometry. The follow-up study of this detached system, TIC 43152097, is based on photometry and high-resolution spectra from the literature and collected by us. The radial velocity of the center of mass and the photospheric lithium abundance of the binary components confirm its membership to NGC 2232. By analyzing the existing photometric and spectroscopic data, we obtain orbital elements and fundamental stellar parameters for the two stars. The primary component of TIC 43152097 is a late F-type dwarf (Teff = 6070 K), while the lower-mass secondary is a late K-type star (Teff = 4130 K) that is still in the pre-main-sequence phase. The precise measurements of the radii, masses, and effective temperatures, enabled by the simultaneous solution of light and radial velocity curves, indicate radius inflation for the K-type component, which turns out to be 7–11% larger than that predicted by standard evolutionary models. More sophisticated models incorporating both the inhibition of convective energy transport caused by sub-photospheric magnetic fields and the effects of cool starspots covering a substantial fraction of the stellar surface (30–60%) allow the position of the secondary component to be reproduced in the Hertzsprung–Russell and mass–radius diagrams.
Key words: binaries: eclipsing / binaries: spectroscopic / stars: low-mass / stars: pre-main sequence / stars: individual: TIC 43152097 / open clusters and associations: individual: NGC 2232
Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Observatorio del Roque de los Muchachos. Based on photometry collected at the INAF – Osservatorio Astrofisico di Catania.
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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