Volume 467, Number 3, June I 2007
|Page(s)||1093 - 1101|
|Section||Interstellar and circumstellar matter|
|Published online||13 March 2007|
The circumbinary disc around the J-type C-star IRAS 18006-3213*
Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium e-mail: email@example.com
2 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
Accepted: 6 March 2007
Context.In the generally accepted, but poorly documented model, silicate J-type C-stars are binary objects for which the silicate emission originates from a circumbinary or a circumcompanion disc.
Aims.We aim at testing this hypothesis by a thorough spectral and spatial observational study of one object: IRAS 18006-3213.
Methods.We obtained, analysed and modeled high spatial resolution interferometric VLTI/MIDI observations on multiple baselines ranging from 45 m to 100 m.
Results.All observations resolved the object and show the very compact nature of the N-band emission (~30 mas). In addition, the highest spatial resolution data show a significant differential phase jump around 8.3 μm. This demonstrates the asymmetric nature of the N-band emission. Moreover, the single telescope N-band spectrum shows the signature of highly processed silicate grains. These data are used to confirm the model on silicate J-type C-stars for IRAS 18006-3213. We show that the most favourable model of the dust geometry is a stable circumbinary disc around the system, seen under an intermediate inclination.
Conclusions.The data presented on the silicate J-type C-star IRAS 18006-3213 provide evidence that the oxygen rich dust is trapped in a circumbinary disc. The formation of this disc is probably linked to the binary nature of the central star.
Key words: techniques: interferometric / stars: AGB and post-AGB / stars: carbon / stars: circumstellar matter / stars: individual: IRAS 18006-3213
© ESO, 2007
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