Volume 412, Number 2, December III 2003
|Page(s)||L43 - L46|
|Published online||28 November 2003|
Letter to the Editor
Evidence for grain growth in T Tauri disks*
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
Corresponding author: F. Przygodda, email@example.com
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]2SiO4) 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
© ESO, 2003
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