Fig. 1.From: Thermal and hydrostatic structure of the protoplanetary disks: Influences of wind strengths, mass distributions, and stellar wind velocity lawsThe flaring index, f, as a function of η for five different cases of t*/ β. In the figure, n denotes the result for the case of t* / β = 1 × 10n yr. We also overwrite the second term, 4/3πη, in the right hand side of Eq. (16) in order to readily see the roles in determining the disk temperature.Back to article page