Fig. 7.From: Thermal and hydrostatic structure of the protoplanetary disks: Influences of wind strengths, mass distributions, and stellar wind velocity lawsThe height and temperature of the disk for the case of t*/β = 1 × 1012 yr. Solid and dashed curves denote the results calculated by vw ∝ r−1/2 and the constant velocity model, respectively.Back to article page