Institut für Astronomie und Astrophysik
Abteilung AstronomieSand 1, D-72076 Tübingen, Germany
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Rauch, T. (1, 2)
(1) Dr.-Remeis-Sternwarte, Sternwartstraße 7, D-96049 Bamberg, Germany
(2) Institut für Astronomie und Astrophysik, Sand 1, D-72076 Tübingen, Germany
To be published in: The ASP Conference Series (San Francisco: ASP)
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 (~ 0.066 Msun) - formally a brown dwarf. The brown dwarf may have been a former planet which survived a common envelope (CE) phase and has even gained mass.
A recent determination of the components' masses from results of NLTE spectral analysis and subsequent comparison to evolutionary tracks shows a discrepancy to masses derived from radial-velocity and the eclipse curves. Phase-resolved high-resolution and high-SN spectroscopy was carried out in order to investigate on this problem.
We present results of a NLTE spectral analysis of the primary, an analysis of its orbital parameters, and discuss possible evolutionary scenarios.
Key words: stars: binaries: eclipsing - stars: common envelope - stars: evolution - stars: individual: AA Dor - stars: low-mass, brown dwarfs
Preprint (167 kb PDF file including figures)
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Last modified 30 Jan 2013