• The blue curve is from Lindal et al.^[1].

• The green curve is from Bishop et al.^[2]

• The dashed blue curve is an extrapolation of the 1987 Lindal et al. data^[1] using a constant lapse rate of 0.82 K/km.

• The graph also shows locations of the main cloud and haze layers according to 1990 Bishop et al.^[2], Atreya et al.^[3] and dePater et al. ^[4]

References

1. ↑ ^{a b} Lindal, G.F., Lyons, J.R., Sweetnam, D.N., Eshleman, V.R., Hinson, D.P., Tyler, G.L., 1987. The atmosphere of Uranus: Results of radio occultation measurements with Voyager 2. J. Geophys. Res. 92, 14987–15001 (Table 1);
2. ↑ ^{a b} Bishop, J.; Atreya, S.K.; Herbert, F.; and Romani, P. (1990). "Reanalysis of Voyager 2 UVS Occultations at Uranus: Hydrocarbon Mixing Ratios in the Equatorial Stratosphere", Icarus 88: 448–463 (Table 1).
3. ↑ Atreya, S.; Egeler, P.; Baines, K. (2006). "Water-ammonia ionic ocean on Uranus and Neptune?", Geophysical Research Abstracts 8: 05179
4. ↑ dePater, Imke; Romani, Paul N.; Atreya, Sushil K. (1991). "Possible Microwave Absorbtion in by H2S gas Uranus’ and Neptune’s Atmospheres", Icarus 91: 220–233.