HR: 1340h
AN: P23B-1362    [Abstracts]
TI: Global Climate Models of Titan, Uranus, and Neptune
AU: * Friedson, A J
EM: Andrew.Friedson@jpl.nasa.gov
AF: Caltech/JPL, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Orton, G
EM: Glenn.Orton@jpl.nasa.gov
AF: Caltech/JPL, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: West, R
EM: Robert.West@jpl.nasa.gov
AF: Caltech/JPL, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AB: We present the formulation of and some results from global climate models for Titan, Uranus, and Neptune. The model for Titan is a fully three-dimensional, modified version of NCAR's terrestrial global climate model, CAM-3. It includes forcing by Saturn's gravitational tides, a treatment of the planetary boundary layer and surface interactions, scattering and absorption of short-wave radiation, and absorption and emission of long-wave radiation. The physical properties and distribution of aerosols are constrained by Cassini observations. The climate models for Uranus and Neptune are two-dimensional, radiative-diffusive models which calculate sensible heat fluxes and latent-heat fluxes due to ortho-para hydrogen conversion in terms of a mixing-length formulation. The vertical pressure range in these models extends from 100 bars up to 0.1 mbar. Our main goal for the 2-d models is to establish the relative roles of sensible and ortho-para latent-heat fluxes in transporting heat laterally and vertically. We are also currently developing three-dimensional models of Uranus and Neptune based on modification of CAM-3. We will discuss how the parameterization of heat fluxes in the 2-d models can be adapted to model small-scale convection in the presence of ortho-para conversion in the 3-d models. This research is supported by the NASA Outer Planet Research Program.
DE: 3337 Global climate models (1626, 4928)
DE: 3346 Planetary meteorology (5445, 5739)
DE: 5704 Atmospheres (0343, 1060)
SC: Planetary Sciences [P]
MN: 2007 Fall Meeting