Computer Science – Sound
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p43d1462m&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P43D-1462
Computer Science
Sound
[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [0358] Atmospheric Composition And Structure / Thermosphere: Energy Deposition, [5704] Planetary Sciences: Fluid Planets / Atmospheres, [5729] Planetary Sciences: Fluid Planets / Ionospheres
Scientific paper
The Galileo and the Cassini observations at Jupiter returned a large volume of information about the planet's atmosphere. Some of the results posed new questions that need to be addressed. The energy balance of the jovian thermosphere still presents a problem in our understanding of the nature of the energy source that provides for the observed high thermospheric temperatures. The Galileo probe temperature profile showed an imbedded wavelike structure in the thermosphere. The same pressure region has been also sampled through radio occultations. The derived electron density profiles show a system of several narrow peaks in the lower ionosphere. They too have been successfully modeled as signatures of high altitude atmospheric gravity waves. Atmospheric gravity waves are potentially an important mechanism of energy and momentum transport in Jupiter's upper atmosphere. At the moment we have no direct information about the level of wave activity (rate of wave occurrence , amplitudes, horizontal wavelengths, wave periods, global distribution on the planet, direction of propagation, possible sources of waves) in order to be able to assess the role of atmospheric waves in the dynamics of Jupiter's upper atmosphere. We present a study of the effects of atmospheric gravity waves on the H3+ emission of Jupiter and assess the fisability of wave detection through high resolution infrared spectrometry. This study is in support of the science definition of the planed joint NASA/ESA Europa Jupiter System Mission (EJSM). We have developed a 2-D, time dependent fully nonlinear model of the chemical and the dynamic response of the ionospheric plasma to the propagation of atmospheric gravity waves. The model is coupled with a H3+ radiative transfer model to estimate the magnitude of the expected observable signature in the H3+ IR emission. The detection and the characterization of the gravity wave modes present in the Jovian atmosphere will allow us to estimate the amount of energy and momentum directly deposited in the thermosphere and their role in the meridional circulation and secondary pole-to-equator energy transport. From the model, a list of scientific specifications for a dedicated instrument for EJSM/Ganymede orbiter will be derived, in order to fill technical specifications. An infrared high resolution spectro-imager working in the H3+ emission range (3.5-4 micron) would give access to fine tuned atmospheric sounding. A dedicated observation strategy will allow characterization of atmospheric gravity waves in Jupiter’s thermosphere on a global scale and will answer the questions about the energy transport in the jovian upper atmosphere. This work is supported by CNES and NASA under grant NNX07AF29G issued through the Planetary Atmospheres program.
Barrow John D.
Drossart Pierre
Matcheva Katia I.
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