Issue |
A&A
Volume 687, July 2024
|
|
---|---|---|
Article Number | A256 | |
Number of page(s) | 7 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/202348870 | |
Published online | 17 July 2024 |
Probing the shape of the brown dwarf desert around main-sequence A-F-G-type stars using post-common-envelope WD−BD binaries
1
School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, PR China
e-mail: chenzhliang@mail2.sysu.edu.cn; mabo8@mail.sysu.edu.cn
2
CSST Science Center for the Guangdong-HongKong-Macau Great Bay Area, Sun Yat-sen University, Zhuhai 519082, PR China
3
Yunnan Observatories, Chinese Academy of Sciences, 396 YangFangWang, Guandu District, Kunming 650216, PR China
e-mail: gehw@ynao.ac.cn
4
Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, PO Box 110 Kunming 650216, PR China
5
International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, PR China
Received:
7
December
2023
Accepted:
30
March
2024
Context. Brown dwarfs (BDs) with masses in the range 40−60 MJup are rare around solar-type main-sequence (MS) stars, which gives rise to the brown dwarf desert (BDD). One caveat associated with previous studies of BDD is the relatively limited sample size of MS−BD binaries with accurately determined BD masses.
Aims. We aim to produce a large sample of BD companions with precisely determined masses around MS A-F-G-type stars using observations of post-common-envelope white dwarf (WD)−BD binaries.
Methods. We employed the rapid binary evolution code COMPAS to deduce the properties of MS−BD binary progenitors from post-common-envelope WD−BD binaries. With this method, we increase the sample of directly observed MS−BD binaries, enriching the data available for analyzing the BDD around MS A-F-G-type stars.
Results. Our study opens a new window for studying the shape of the BDD around A-F-G-type MS stars in the short-period regime. We find tentative evidence, albeit with a small sample size, that the “driest” part of the BDD around A-F-G-type stars may extend into an orbital period of several hundred days. More post-common-envelope WD−BD binaries detected in the future will advance our understanding of the BDD around A-F-G-type stars.
Key words: binaries: close / brown dwarfs / white dwarfs
© The Authors 2024
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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