UV Spectroscopy of the Giant Planet Atmospheres with STIS

Details UV Spectroscopy of the Giant Planet Atmospheres with STIS UV Spectroscopy of the Giant Planet Atmospheres with STIS

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8661y&link_type=abstract

HST Proposal ID #8661

Computer Science

Hst Proposal Id #8661 Solar System

Scientific paper

We propose STIS observations of the atmospheres of Jupiter, Saturn, Uranus, and Neptune in the ~1600-3100 Angstrom spectral region. Analysis of these observations will be used to determine the abundance and altitude profiles of gaseous absorbers and aerosols from the millibar region to hundreds of millibars. We will also determine the H_2 ortho/para ratio. Atmospheric properties will be derived through comparison of the observations to synthetic spectra based on model atmospheres and state-of-the-art radiative transfer calculations, that include raman scattering in a rigorous manner. Results from this analysis will be used to investigate photochemical processes in the giant planet atmospheres and to constrain the state of the interiors and the transport rate between the deep interior and visible atmosphere.

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