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The time sequence of 105 spectra covering one full orbital period of AA Dor has been analysed. Direct determination of   V  sin  i   for the sdOB component from 97 spectra outside of the eclipse for the lines Mg  ii  4481 Å and Si  iv  4089 Å clearly indicated a substantially smaller value than estimated before. Detailed modelling of line‐profile variations for eight spectra during the eclipse for the Mg  ii  4481 Å line, combined with the out‐of‐eclipse fits, gave   V  sin  i = 31.8 ± 1.8 km s −1  . The previous determinations of   V  sin  i  , based on the He  ii  4686 Å line, appear to be invalid because of the large natural broadening of the line. With the assumption of the solid‐body, synchronous rotation of the sdOB primary, the measured values of the semi‐amplitude  K  1  and   V  sin  i   lead to the mass ratio   q = 0.213 ± 0.013  which in turn gives  K  2  and thus the masses and radii of both components. The sdOB component appears to be less massive than assumed before,   M  1 = 0.25 ± 0.05 M ⊙  , but the secondary has its mass–radius parameters close to theoretically predicted for a brown dwarf,   M  2 = 0.054 ± 0.010 M ⊙   and   R  2 = 0.089 ± 0.005 R ⊙  . Our results do not agree with the recent determination of V?cković et al. based on a  K  2  estimate from line‐profile asymmetries.

The mass ratio and the orbital parameters of the sdOB binary AA Doradus