2024A&A...687A.256C

Context. Brown dwarfs (BDs) with masses in the range 40-60 M_Jup 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.