All Tables

Table 1: Composition of the dust mixture in the outer regions of a protoplanetary accretion disk according to Pollack et al. (1994). The table shows the fraction of the indicated elements condensed into the different dust species. x denotes the mole fraction of the pure magnesium silicate end members of the solid solution series forming the magnesium-iron-silicates called olivine-type and pyroxene-type, respectively, on the basis of their assumed chemical composition. Only those dust components of the most abundant refractory elements are considered that are the main sources of dust opacity.
Table 2: Coefficients required for calculating evaporation and condensation rates. Data for $\rho$ and A from the CRC-handbook (Lide 1995). For V₀ and $\alpha$ see text.
Table 3: Parameters used for the calculation of the disc model.
Table 4: Composition of the silicate mixture at 3 and 20 AU in a stationary protoplanetary disc model with $\dot M=1\times 10^{-7}~M_{\odot}$ yr^-1. The numbers are fractions of the silicon contained in the different dust species. "cr'' and "am'' denote crystalline dust or amorphous dust with a composition like that of the indicated crystalline material, respectively.