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AA DOR An Eclipsing Subdwarf - Brown Dwarf Binary

Published online by Cambridge University Press:  22 February 2018

T. Rauch
T. Rauch*
Affiliation:
Dr.-Remeis-Sternwarte, Sternwartstraße 7, D-96049 Bamberg, Germany ([email protected]) Institut für Astronomie und Astrophysik, Sand 1, D-72076 Tübingen, Germany

Extract

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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⊙.

Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 246
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Driebe, T., Schönberner, D., Blöcker, T., & Herwig, F. 1998. A&A, 339, 129 Google Scholar
Hilditch, R.W., Kilkenny, D.. & Lynas-Gray, A.E., Hill, G. 2003. MNRAS, 344, 644 CrossRefGoogle Scholar
Rauch, T. 2000. A&A, 356, 665 Google Scholar
Rauch, T. 2004. Ap&SS. in pressGoogle Scholar
Rauch, T., & Werner, K. 2003. A&A., 400, 271 Google Scholar