Dust Growth and Settling in Protoplanetary Disks and Disk Spectral Energy Distributions. I. Laminar Disks

Abstract

Dust growth and settling considerably affect the spectral energy distributions (SEDs) of protoplanetary disks. We investigated dust growth and settling in protoplanetary disks through numerical simulations to examine time-evolution of the disk optical thickness and SEDs. In the present paper, we considered laminar disks as a first step of a series of papers. As a result of dust growth and settling, a dust layer forms around the mid-plane of a gaseous disk. After the formation of the dust layer, small dust grains remain floating above the layer. Although the surface density of the floating small grains is much less than that of the dust layer, they govern the disk optical thickness and the emission. The floating small grains settle onto the dust layer in a long time scale compared with the formation of the dust layer. Rapid grain growth in the inner part of disks makes the radial distribution of the disk optical thickness less steep than that of the disk surface density. At t > 10^6yr, the optical thickness of the inner disk (> a few AU) almost vanishes, which may correspond to disk inner holes observed by Spitzer Space Telescope. Furthermore, we examined time-evolution of disk SEDs, using our numerical results and the two-layer model. The grain growth and settling decrease the magnitude of the SEDs especially. Our results indicate that grain growth and settling can explain the decrease in observed energy fluxes at millimeter/sub-millimeter wavelengths with time scales of 10^{6-7}yr without depletion of the disks.