New analysis of the Voyager UVS H Lyman-alpha emission of Saturn

Details New analysis of the Voyager UVS H Lyman-alpha emission of Saturn New analysis of the Voyager UVS H Lyman-alpha emission of Saturn

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995icar..113...91b&link_type=abstract

Icarus (ISSN 0019-1035), vol. 113, no. 1, p. 91-102

Physics

13

Emission Spectra, Hydrogen, Lyman Alpha Radiation, Saturn (Planet), Voyager Project, Airglow, Radiative Transfer, Rayleigh Scattering, Ultraviolet Spectrometers

Scientific paper

The limb to limb Lyman-alpha reflectivities observed with the Voyager ultraviolet spectrometer (UVS) instruments during the fly-by of Saturn are reanalyzed using a revised H Lyman-alpha sensitivity for the Voyager 1 instrument. The new sensitivity reconciles the measured intensities to those of Voyager 2 and gives a coherent set of data. To fit the UV airglow observations, four sources are considered: (1) H resonance and H2 Rayleigh scattering of solar Lyman-alpha radiation, (2) the interplanetary Lyman-alpha radiation, (3) a possible internal source of unknown origin, (4) the possibility of atmospheric turbulence recently proposed to explain the Lyman-alpha bulge of Jupiter. The analysis supports neither a dominant collisional excitation source for the UV emissions nor the presence of strong atmospheric turbulence. The best fit, in terms of brightness but also in terms of shape of the limb to limb profile (that is to say independent on the absolute calibrations), is obtained for pure resonance and Rayleigh scattering of solar and interstellar wind line in an atmosphere enriched in atomic hydrogen up to three times the standard model. Influx of water from the rings of Saturn may provide a means for producing such enhanced H densities in the upper atmosphere.

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