Constraints on the Radial Variation of Grain Growth in the AS 209 Circumstellar Disk

We present dust continuum observations of the protoplanetary disk surrounding the pre-main sequence star AS 209, spanning more than an order of magnitude in wavelength from 0.88 to 9.8 mm. The disk was observed with sub-arcsecond angular resolution (0.2"-0.5") to investigate radial variations in its dust properties. At longer wavelengths, the disk emission structure is notably more compact, providing model-independent evidence for changes in the grain properties across the disk. We find that physical models which reproduce the disk emission require a radial dependence of the dust opacity \kappa_{\nu}. Assuming that the observed wavelength-dependent structure can be attributed to radial variations in the dust opacity spectral index (\beta), we find that \beta® increases from \beta<0.5 at \sim20 AU to \beta>1.5 for R>80 AU, inconsistent with a constant value of \beta\ across the disk (at the 10\sigma
level). Furthermore, if radial variations of \kappa_{\nu} are caused by particle growth, we find that the maximum size of the particle-size distribution (a_{max}) increases from sub-millimeter-sized grains in the outer disk (R>70 AU) to millimeter and centimeter-sized grains in the inner disk regions (R< 70 AU). We compare our observational constraint on a_{max}® with predictions from physical models of dust evolution in proto-planetary disks. For the dust composition and particle-size distribution investigated here, our observational constraints on a_{max}® are consistent with models where the maximum grain size is limited by radial drift.