Statistics – Computation
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phdt........31s&link_type=abstract
PhD Dissertation, Cornell Univ. New York, NY United States
Statistics
Computation
2
Radiative Transfer, Neptune Atmosphere, Uranus Atmosphere, Mars Atmosphere, Venus Atmosphere, Solar Wind, Magnetohydrodynamic Waves, Solar Wind Velocity, Velocity Distribution, Galileo Spacecraft, Mariner 9 Space Probe, Aerosols, Algorithms, Para Hydrogen, Venus Clouds, Ortho Hydrogen, Three Dimensional Models, Scattering, Lapse Rate, Temperature Effects, Space Plasmas, Infrared Spectra
Scientific paper
A variety of projects involving dynamics and radiation in planetary atmospheres are presented. The cloud-top wind field of Venus is explored by tracking clouds and by measuring the shape and orientation of the streaky clouds. Cloud-tracked winds from Galileo images show a prominent global-scale oscillation in the zonal wind with amplitude 10 m/s-1 and period 4 days. The variation with longitude of cloud orientations indicates that solar thermal tides have an amplitude roughly twice as large as the Hadley circulation, producing equatorward meridional velocities on the night side of Venus. A linear 3-D model of the Venus atmosphere with spherical geometry is used to study global-scale waves. When a radiative-dynamic cloud feedback is added, the most unstable wavemode is found to have the same phase speed and horizontal structure as the observed Galileo oscillation. A radiative transfer computation including aerosol scattering is carried out for Mars. An algorithm for the retrieval of the extinction coefficient and single scattering albedo from infrared spectra is developed for future spacecraft missions. Preliminary retrieval algorithms are explored for Mariner 9 IRIS and ground-based infrared spectra. Convection in the outer planets including the thermodynamics of para and ortho hydrogen is modeled by extending the convective adjustment scheme used in terrestrial models. The delayed equilibration of hydrogen leads to intermittent convection on Uranus and Neptune, a new result. For Jupiter, the influence of hydrogen equilibration is small and has little effect on convection. For Uranus and Neptune, the model predicts a para fraction near equilibrium, and a temperature lapse rate between the intermediate and equilibrium adiabats, both as observed.
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