On the analysis of the H Lyman-alpha dayglow of Jupiter, Saturn and Uranus

Details On the analysis of the H Lyman-alpha dayglow of Jupiter, Saturn and Uranus On the analysis of the H Lyman-alpha dayglow of Jupiter, Saturn and Uranus

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993p%26ss...41..363e&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 41, no. 5, p. 363-371.

Computer Science

6

Dayglow, H Alpha Line, Jupiter Atmosphere, Lyman Alpha Radiation, Saturn Atmosphere, Uranus Atmosphere, Gas Density, Iue, Radiative Transfer, Planets, Outer Planets, Gas Planets, Lyman Alpha Radiation, Hydrogen, Jupiter, Saturn, Uranus, Analysis, Atmosphere, Model, Atmosphere, Radiative Transfer, Airglow, Emissions, Scattering, Simulation, Shape, Intensity, Dynamics, Eddy Diffusion, Density, Turbulence, Comparison, Spacecraft Observations

Scientific paper

A new radiative transfer model, particularly well adapted to calculations in inhomogeneous atmospheres, has been applied, during the last four years, to analyze new and older Lyman-alpha airglow data from three giant planets. We review all the results obtained so far. Several features which were not accounted for by using the previous transfer codes were satisfactorily simulated, using essentially the scattering of the solar and the interplanetary Lyman-alpha lines by hydrogen in the upper atmospheres. The search for a good fit both in intensity and in shape of the limb to limb data, and/or of the line profiles, provided constraints on the dynamics of the atmospheres, through the estimate of either the eddy diffusion coefficient, the total H column density, or of the possibility of some nonthermal turbulence processes at high altitude. Consequently, the need for an 'electroglow' process for the Lyman-alpha emission was considerably reduced and may be dismissed in the majority of cases.

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