Examples of how the temperature power law affects the radius derived from the brightness profile. For each line, the left models show the results from a flat disk (power-law exponent −3/4; Chiang & Goldreich 1997), while the right models show the results assuming a flared disk (power-law exponent −3/7; D’Alessio et al. 1999). The difference is larger for lines with higher transition probabilities (A_ki = 9.3e6 s⁻¹ for FeI 6400 Å,A_ki = 5.6e4 s⁻¹ for FeI 6462 Å) that are likely to be formed higher over the disk midplane. Colors and symbols as in Fig. 13.