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Context: Circumstellar disks are considered to be the environment for theformation of planets. The growth of dust grains in these disks is the firststep in the core accretion-gas capture planet formation scenario. Indicatorsand evidence of disk evolution can be traced in spatially resolved images andthe spectral energy distribution (SED) of these objects.  Aims: We develop a model for the dust phase of the edge-on orientedcircumstellar disk of the Butterfly Star which allows one to fit observedmulti-wavelength images and the SED simultaneously.  Methods: Our model is based on spatially resolved high angular resolutionobservations at 1.3 mm, 894 micron, 2.07 micron, 1.87 micron, 1.60 micron, and1.13 micron and an extensively covered SED ranging from 12 micron to 2.7 mm,including a detailed spectrum obtained with the Spitzer Space Telescope in therange from 12 micron to 38 micron. A parameter study based on a grid searchmethod involving the detailed analysis of every parameter was performed toconstrain the disk parameters and find the best-fit model for the independentobservations. The individual observations were modeled simultaneously, usingour continuum radiative transfer code.  Results: We derived a model that is capable of reproducing all of theobservations of the disk at the same time. We find quantitative evidence forgrain growth up to ~100 micron-sized particles, vertical settling of largerdust grains toward the disk midplane, and radial segregation of the lattertoward the central star. Within our best-fit model the large grains have adistribution with a scale height of 3.7 AU at 100 AU and a radial extent of 175AU compared to a hydrostatic scale height of 6.9 AU at 100 AU and an outer diskradius of 300 AU. Our results are consistent with current theoretical modelsfor the evolution of circumstellar disks and the early stages of planetformation.

Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star