Far UV Observations of the Giant Planets - Cycle 0

Details Far UV Observations of the Giant Planets - Cycle 0 Far UV Observations of the Giant Planets - Cycle 0

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990hst..prop.1269p&link_type=abstract

HST Proposal ID #1269

Physics

Hst Proposal Id #1269

Scientific paper

H and H2 are the main constituents of the upper atmospheres of the giant planets and Titan, H is abundant in their exospheres and magnetospheres and N2, produced by photolysis of NH3, dominates the lower atmosphere of Titan. The spatial distribution of these elements is determined by the photochemical and particle dissociation processes responsible for their production and by the transport mechanisms responsible for their distribution. The presence of these planetary constituents is revealed by emissions of the HI, 1216 A Lyman alpha line, the H2 Lyman and Werner, and the N2 Lyman-Birge-Hopfield bands in the 1000-2000A region, all produced by particle impact excitation and/or resonance scattering of sunlight. Spatial and spectral images of the H, H2 and N2 atmospheres around these objects, consequently, represent key diagnostic tools in the investigation of these fundamental planetary phenomena. Moreover, Lyman alpha images of the giant planets taken at high enough spatial resolution will permit a determination of the abundance of deuterium, an extremely sensitive tracer of primordial nucleosynthesis. We propose to obtain a series of high resolution images of the giant planets' upper atmospheres and near-planetary environments in the far uv that are unobtainable from the ground or from the present generation of planetary probes.

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