Computer Science – Databases
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsa41c..02b&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SA41C-02
Computer Science
Databases
3369 Thermospheric Dynamics (0358), 5409 Atmospheres: Structure And Dynamics, 5707 Atmospheres: Structure And Dynamics, 6207 Comparative Planetology
Scientific paper
The comparative approach to planetary aeronomy is becoming increasingly fruitful as new information from various planet atmospheres is assimilated. Various planetary thermospheric observations and modeling over the past 35-years provide a useful platform for addressing similar upper atmosphere processes (thermal, dynamical, chemical) in various planetary settings. Planetary upper atmospheres can be roughly catagorized as those imbedded in their own planetary magnetosphere (e.g. Earth and Jupiter) and those that are not (e.g. Venus, Mars, Titan). This distinction determines the different thermospheric heating mechanisms that generally dominate for magnetic (auroral and Joule heating) and non-magnetic (solar EUV/UV heating) bodies. In addition, other basic features of the structure and dynamics of the Venus, Earth, Mars, Jupiter and Titan thermospheres can be understood by examining the implications of their fundamental planetary parameters (e.g. radius, gravity, heliocentric distance, rotation rate). The present maturity of available Venus and Earth planetary databases (and the promise for Mars) as well as numerical modeling capabilities permit us to compare the thermospheres of Venus, Earth, and Mars using well tested and individually validated three-dimensional (3-D) thermospheric general circulation models (TGCMs). Recently developed Jupiter and Titan TGCMs also reveal unique characteristics of their thermospheric winds and structures that data have yet to confirm. We present sample TGCM simulations that capture the physics of these 5-thermospheres. Clearly, our geocentric perspective when applied to other planet atmospheres is initially helpful. However, investigations must be revised as new planetary data and model simulations combine to challenge our understanding of aeronomic processes in new planetary environments.
Bougher Stephen W.
Muller-Wodarg I. C.
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