Gravity Waves in Jupiter's Upper Atmosphere

Details Gravity Waves in Jupiter's Upper Atmosphere Gravity Waves in Jupiter's Upper Atmosphere

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.2105y&link_type=abstract

American Astronomical Society, DPS meeting #28, #21.05; Bulletin of the American Astronomical Society, Vol. 28, p.1134

Astronomy and Astrophysics

Astronomy

Scientific paper

The Atmospheric Structure Instrument (ASI) on the Galileo Probe measured the temperature profile of Jupiter's atmosphere from a few nbar to a few bars. For the first time, there exists an accurate temperature profile of a giant planet thermosphere. The temperature gradients in Jupiter's thermosphere are large (2-3 K/km) and sustained; the maximum temperature reached is a surprising 1300 K at 4 nbar (920 km above the 1-bar level). To maintain this high temperature and steep gradient, there must be an energy source high in the thermosphere. Gravity waves have been proposed previously as a source of heating in Jupiter's thermosphere. In particular, small-scale (5 K) fluctuations in Jupiter's upper atmosphere have been seen in stellar occultations and have been interpreted as breaking gravity waves with vertical wavelengths near 13 km. These fluctuations are not observed much higher than the homopause. A different class of fluctuations are seen in the ASI temperature profile, with long wavelengths, and large amplitudes. If these are waves, they have amplitudes of 12-35 K and vertical wavelengths of 50-75 km. These fluctuations begin in the stratosphere, and, unlike the short-wavelength fluctuations, are easily seen nearly to the 20-nbar level, several hundred km above the homopause. Can gravity-wave heating produce the observed thermal profile? Why do the short-wavelength waves seem to disappear above the homopause, while the long-wavelength waves continue to be present? To answer these questions, we numerically solve the gravity wave equations. We use the thermal profile measured by the ASI, rigorously include molecular viscosity and thermal conduction, and do not assume that the waves are in hydrostatic equilibrium (so that the frequency can approach the Brunt-Vaisala frequency). We will discuss propagation and energy transport for thermospheric gravity waves with a variety of vertical wavelengths and periods.

Affiliated with

Also associated with

No associations

Rating

Gravity Waves in Jupiter's Upper Atmosphere does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Gravity Waves in Jupiter's Upper Atmosphere, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Gravity Waves in Jupiter's Upper Atmosphere will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1461932