Abstract
Abstract We present the results of age determination for galactic B-type main-sequence stars that are components of double-lined eclipsing binaries. Only detached systems are considered. We analyze 38 binary systems that meet such criteria. The analysis is based on evolutionary computations, and we consider that the age is determined if there is a common value from the radius–age diagrams and the agreement in the position of both components in the Hertzsprung–Russell diagram. In some cases, to meet these two conditions, it was necessary to adjust the value of the metallicity, Z, or/and the parameter of overshooting from the convective core, α ov. We determine a consistent age for 33 of the 38 binaries. Additionally, we completed extensive computations, and for each system, we give the range of α ov and Z for which a consistent solution exists. The age of the studied B-type main-sequence stars ranges, as counted from the Zero Age Main Sequence, from about 2.5 Myr to about 200 Myr.
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