Evidence for grain growth in T Tauri disks
Frank PrzygoddaMax-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, GermanyR. van BoekelAstronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The NetherlandsP. ÁbrahámKonkoly Observatory of the Hungarian Academy of Sciences, 1525 Budapest, PO Box 67, HungaryS. MelnikovUlugh Beg Astronomical Institute, Academy of Sciences of Uzbekistan, Astronomical str. 33, Tashkent 700051, UzbekistanL. B. F. M. WatersInstituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Heverlee, BelgiumCh. LeinertMax-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
ABI
Аннотация
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.
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