Jupiter - Structure and composition of the upper atmosphere

Details Jupiter - Structure and composition of the upper atmosphere Jupiter - Structure and composition of the upper atmosphere

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...247l..43a&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 247, July 1, 1981, p. L43-L47. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

79

Atmospheric Composition, Atmospheric Heating, Atmospheric Temperature, Jupiter Atmosphere, Temperature Distribution, Turbulent Diffusion, Atmospheric Chemistry, Density Distribution, Exosphere, Mesosphere, Particle Precipitation, Plasma Heating, Stellar Occultation, Ultraviolet Spectrometers, Voyager Project, Jupiter, Structure, Composition, Atmosphere, Voyager 1, Temperatures, Wavelengths, Ammonia, Clouds, Gradients, Mesosphere, Ions, Density, Heating, Magnetosphere, Charged Particles, Gravity Waves, Exper

Scientific paper

The Voyager ultraviolet stellar occultation data yield a temperature of 200 + or - 50 K at about 400 km, and the solar occultation data give 1100 + or - 200 K at 1450 km above the ammonia cloud tops. The temperature gradient between 400 and 1450 km is approximately 1 K/km. The mesospheric temperature structure gives no strong indication of an earth-like mesopause. The heating of the upper atmosphere appears to result from a combination of magnetospheric charged particle precipitation, ion drag, inertia gravity waves, and solar EUV. The volume mixing ratios of CH4 and C2H6 at 325 km are measured to be 2.5(+3, -2) x 10 to the -5th and 2.5(+2.0, -1.5) x 10 to the -6th, respectively, which are lower than in the stratosphere. The C2H2 volume mixing ratio is not greater than 5 x 10 to the -6th at 300 km. The homopause value of the equatorial eddy diffusion coefficient is found to be 1-2 x 10 to the -6th sq cm/s.

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