Volume 446, Number 1, January IV 2006
|Page(s)||211 - 221|
|Section||Interstellar and circumstellar matter|
|Published online||09 January 2006|
Large dust particles in disks around T Tauri stars
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany e-mail: firstname.lastname@example.org
2 National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801, USA
3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA
4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Accepted: 14 September 2005
We present 7-mm continuum observations of 14 low-mass pre-main-sequence stars in the Taurus-Auriga star-forming region obtained with the Very Large Array with ~15 resolution and ~0.3 mJy rms sensitivity. For 10 objects, the circumstellar emission has been spatially resolved. The large outer disk radii derived suggest that the emission at this wavelength is mostly optically thin. The millimetre spectral energy distributions are characterised by spectral indices 2.3 to 3.2. After accounting for contributions from free-free emission and corrections for optical depth, we determine dust opacity indices β in the range 0.5 to 1.6, which suggest that millimetre-sized dust aggregates are present in the circumstellar disks. Four of the sources with may be consistent with submicron-sized dust as found in the interstellar medium. Our findings indicate that dust grain growth to millimetre-sized particles is completed within less than 1 Myr for the majority of circumstellar disks.
Key words: stars: pre-main sequence / stars: planetary systems: protoplanetary disks / planetary systems: formation
© ESO, 2006
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