Issue |
A&A
Volume 446, Number 1, January IV 2006
|
|
---|---|---|
Page(s) | 211 - 221 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20054038 | |
Published online | 09 January 2006 |
Large dust particles in disks around T Tauri stars
1
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany e-mail: rodmann@mpia.de
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
Received:
12
August
2005
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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