Abstract
AA DOR, is an eclipsing, close, post common-envelope binary (PCEB) consisting of a sdOB primary star and an unseen secondary with an extraordinary small mass (M2 ≈ 0.066M⊙) formally a brown dwarf (see Rauch 2004 for details). In a spectral analysis of AA DOR, Rauch (2000) determined Teff = 42 kK and log g — 5.2 (cgs). The determination of the components' masses by comparison of these results with evolutionary models of Driebe et al. (1998) shows a discrepancy to masses derived from radial-velocity and the eclipse curves (Hilditch et al. 2003) log g = 5.5 would be necessary in order to achieve an intersection at M1 ≈ 0.330M⊙.
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