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Partial frequency redistribution (PRD), describing the formation of the lineprofile, has negligible observational effects for optical depths smaller than~10^3, at the resolving power of most current instruments. However, when thespectral resolution is sufficiently high, PRD modeling becomes essential ininterpreting the line shapes and determining the total line fluxes. Wedemonstrate the effects of PRD on the H_2 line profiles observed at highspectral resolution by the Far-Ultraviolet Spectroscopic Explorer (FUSE) in theatmospheres of Jupiter and Saturn. In these spectra, the asymmetric shapes ofthe lines in the Lyman (v"- 6) progression pumped by the solar Ly-beta areexplained by coherent scattering of the photons in the line wings. We introducea simple computational approximation to mitigate the numerical difficulties ofradiative transfer with PRD, and show that it reproduces the exact radiativetransfer solution to better than 10%. The lines predicted by our radiativetransfer model with PRD, including the H_2 density and temperature distributionas a function of height in the atmosphere, are in agreement with the lineprofiles observed by FUSE. We discuss the observational consequences of PRD,and show that this computational method also allows us to include PRD inmodeling the continuum pumped H_2 fluorescence, treating about 4000 linessimultaneously.

Observations and modeling of H_2 fluorescence with partial frequency redistribution in giant planet atmospheres