Abstract
A model of the atmospheric structure of Uranus is presented which differs from previous types of models in two important respects: (1) The CH 4/H 2 ratio is sufficiently large that CH 4 is saturated to large depths in the Uranian atmosphere. (2) The internal energy flux is small compared with that due to solar heating. Because of the small internal flux, the thermal flux decreases rapidly with depth and the atmosphere is radiative to large optical depths. A CH 4 droplet cloud forms where the atmosphere finally becomes convective due to the internal flux. The model is shown to be in reasonable agreement with published observations of the H 2 quadrupole 3-0 and 4-0 bands, the visible (4000–6000 Å) CH 4 bands, and the infrared emission spectrum.
Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
