EDP Sciences
Free Access
Volume 401, Number 2, April II 2003
Page(s) 577 - 592
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20030043
Published online 21 March 2003

A&A 401, 577-592 (2003)
DOI: 10.1051/0004-6361:20030043

The origin of crystalline silicates in the Herbig Be star HD 100546 and in comet Hale-Bopp

J. Bouwman1, 2, A. de Koter1, C. Dominik1 and L. B. F. M. Waters1, 3

1  Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2  CEA, DSM, DAPNIA, Service d'Astrophysique, CE Saclay, 91191 Gif-sur-Yvette Cedex, France
3  Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200 B, 3001 Heverlee, Belgium

(Received 8 April 2002 / Accepted 9 January 2003 )

We have investigated the spatial distribution, and the properties and chemical composition of the dust orbiting HD 100546. This system is remarkably different from other isolated Herbig Ae/Be stars in both the strength of the mid-IR excess and the composition of the circumstellar dust. To explain spectral features and the amount of mid-IR dust emission

the presence of a component of small ( <10  $\mu$m) grains radiating at ~200 K is required, which is not seen in other well investigated Herbig Ae/Be systems. This additional component is inconsistent with a uniform flaring disk model. The fraction of intercepted stellar light that is absorbed and re-emitted in the mid-IR is so large (~70%) that it requires the disk to be more "puffed up" at about 10 AU, where the grains have $T \sim 200$ K. This may occur if a proto-Jupiter clears out a gap at this distance allowing direct stellar light to produce an extended rim at the far side of the gap. The other remarkable difference with other isolated Herbig Ae/Be systems is the presence of a much larger mass fraction of the crystalline silicate forsterite in the circumstellar dust. We find that the mass fraction of crystalline silicates in HD 100546 increases with decreasing temperature, i.e. with larger radial distances from the central star. This distribution of crystalline dust is inconsistent with radial mixing models where the crystalline silicates are formed by thermal annealing above the glass temperature in the very inner parts of the disk, and are subsequently transported outwards and mixed with amorphous material. We speculate that the formation and spatial distribution of the crystalline dust may be linked to the formation of a proto-Jupiter in the disk around HD 100546. Such a proto-Jupiter could gravitationally stir the disk leading to a collisional cascade of asteroidal sized objects producing small crystalline grains, or it could cause shocks by tidal interaction with the disk which might produce crystalline dust grains through flash heating. As shown by Malfait et al. (1998), the infrared spectrum of HD 100546 is very similar to that of C/1995 O1 Hale-Bopp (Crovisier et al. 1997). Using an identical methodology, we have therefore also studied this solar system comet. Both objects have an almost identical grain composition, but with the important difference that the individual dust species in Hale-Bopp are in thermal contact with each other, while this is not the case in HD 100546. This suggests that if similar processes leading to the dust composition as seen in HD 100546 also occurred in our own solar system, that Hale-Bopp formed after the formation of one or more proto-gas giants.

Key words: circumstellar matter -- stars: formation -- stars: pre-main-sequence

Offprint request: J. Bouwman, jeroenb@astro.uva.nl

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