Fig. 5.From: Thermal and hydrostatic structure of the protoplanetary disks: Influences of wind strengths, mass distributions, and stellar wind velocity lawsDependence of the flaring index, f (panel (a)), the disk height, zs (panel (b)), and the temperature, T (panel (c)), on the power-law index γ which characterizes the mass distribution (see Eq. (1)). As for t*/ β, we take this as 1 × 1012 yr.Back to article page