EDP Sciences
Free access
Volume 412, Number 2, December III 2003
Page(s) L43 - L46
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20034606

A&A 412, L43-L46 (2003)
DOI: 10.1051/0004-6361:20034606


Evidence for grain growth in T Tauri disks

F. Przygodda1, R. van Boekel2, P. Àbrahàm3, S. Y. Melnikov4, L. B. F. M. Waters2, 5 and Ch. Leinert1

1  Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
2  Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
3  Konkoly Observatory of the Hungarian Academy of Sciences, 1525 Budapest, PO Box 67, Hungary
4  Ulugh Beg Astronomical Institute, Academy of Sciences of Uzbekistan, Astronomical str. 33, Tashkent 700051, Uzbekistan
5  Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium

(Received 9 September 2003 / Accepted 5 November 2003)

In this article we present the results from mid-infrared spectroscopy of a sample of 14 T Tauri stars with silicate emission. The qualitative analysis of the spectra reveals a correlation between the strength of the silicate feature and its shape similar to the one which was found recently for the more massive Herbig Ae/Be stars by van Boekel et al. (2003). The comparison with theoretical spectra of amorphous olivine ([Mg,Fe] 2SiO 4) with different grain sizes suggests that this correlation is indicating grain growth in the disks of T Tauri stars. Similar mechanisms of grain processing appear to be effective in both groups of young stars.

Key words: stars: pre-main sequence -- stars: planetary systems: protoplanetary disks -- stars: circumstellar matter

Offprint request: F. Przygodda, przygodda@mpia.de

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© ESO 2003

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