Low-latitude H Lyman-alpha emissions from the Galileo Ultraviolet Spectrometer

Details Low-latitude H Lyman-alpha emissions from the Galileo Ultraviolet Spectrometer Low-latitude H Lyman-alpha emissions from the Galileo Ultraviolet Spectrometer

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997dps....29.1604t&link_type=abstract

American Astronomical Society, DPS meeting #29, #16.04; Bulletin of the American Astronomical Society, Vol. 29, p.997

Astronomy and Astrophysics

Astronomy

Scientific paper

The processes contributing to the detailed formation of H Lyman-alpha emission in Jupiter's upper atmosphere at low latitudes are still not thoroughly known although resonant scattering of solar H Lyman-alpha photons, charged particle collisional excitation of H, dissociative exitation of H2, and hydrogenic ion recombination (H+ or H3+) have been proposed. The Galileo Ultraviolet Spectrometer (UVS) has systematically observed Jupiter's low latitude hydrogen Lyman-alpha during the first half of the prime mission. Observations from orbits G1 through G8 have provided a preliminary mapping of the Lyman-alpha distribution for most System III longitudes. These observations provide a database for examining the contribution of many of the formation mechanisms because emissions related to solar and non-solar processes are separately observed away from the auroral zones across most longitudes and for most emission angles. The Galileo UVS H Lyman-alpha data are shown and possible production mechanisms are suggested for the observed emissions.

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