Morphology of infrared H3(+) emissions in the auroral regions of Jupiter

Details Morphology of infrared H3(+) emissions in the auroral regions of Jupiter Morphology of infrared H3(+) emissions in the auroral regions of Jupiter

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992icar...97...10d&link_type=abstract

Icarus (ISSN 0019-1035), vol. 97, no. 1, May 1992, p. 10-25.

Astronomy and Astrophysics

Astronomy

29

Astronomical Maps, Auroral Zones, Emission Spectra, Hydrogen Ions, Jupiter Atmosphere, Acetylene, Astronomical Models, Infrared Astronomy, Iue, Methane

Scientific paper

It is possible, on the basis of a careful analysis of Jupiter's 4-micron emission, to describe the morphology of the auroral emission in H3(+), which occurs above a background of both thermal emission and sunlight reflection by the clouds and hazes of Jupiter. This emission's structure is strongly peaked in auroral spots. These results differ from those of Baron et al. (1991), which pointed to H3(+) emission poleward of the auroral oval. The data-reduction procedure used here includes continuum subtraction, thereby enhancing confidence that the H3(+) emission in the data set did not extend poleward of the auroral oval at the date of the observations.

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