Variability of Lyman-alpha emission from Jupiter

Astronomy and Astrophysics – Astronomy

Scientific paper

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Emission Spectra, Jupiter Atmosphere, Lyman Alpha Radiation, Planetary Radiation, Hydrogen Atoms, Line Spectra, Solar Activity Effects, Ultraviolet Astronomy, Jupiter, Emission, Lyman-Alpha Radiation, Spectrometer, Oao 3, Atmosphere, Hydrogen, Ultraviolet Radiation, Spectrum, Solar Activity, Dissociation, Methane, Comparisons, Equipment, Doppler Effect, Data, Techniques, Observations, Data Reduction, Intensity, Scattering, Density, Models, Mesopause, Thermosphere

Scientific paper

The Jovian Lyman-alpha emission line was reobserved in 1978 March using the high-resolution spectrometer of the Copernicus satellite. An intensity of 8.3 plus or minus 2.9 kilorayleighs was measured. This value represents a significant increase in intensity over previous (1976) Copernicus observations, but is lower than the recent (1979) values obtained by Voyager 1 and IUE. The increase in intensity has been accompanied by a significant increase in line width giving strong support to the theory that the emission results from resonant scattering of the solar Lyman-alpha line by H atoms in the upper Jovian atmossphere. The strength of Jovian Lyman-alpha emission correlates well with the level of solar activity. The solar extreme ultraviolet radiation varies with the solar cycle. This radiation causes the dissociation of H2 and CH4 into H atoms in the Jovian atmosphere. Therefore, in times of high solar activity, the H column density will increase, causing the observed strong Jovian Lyman-alpha emission.

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