Magnetosphere-Ionosphere-Thermosphere coupling and the Energy Crisis at Saturn

Details Magnetosphere-Ionosphere-Thermosphere coupling and the Energy Crisis at Saturn Magnetosphere-Ionosphere-Thermosphere coupling and the Energy Crisis at Saturn

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1432m&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1432

Computer Science

Scientific paper

We have updated the Saturn Thermosphere Ionosphere Model (STIM) to more comprehensively calculate processes of magnetosphere-ionospherethermosphere coupling, including self-consistent calculation of energetic particle precipitation and the resulting energy deposition [2], resulting in polar ionization. Furthermore, the ionosphere, unlike in previous calculations, is now fully dynamically coupled to the thermosphere. Previous calculations [3] using the same ionosphere component of STIM have shown that best agreement between Total Electron Content values from STIM and Cassini Radio Science Subsystem (RSS) observations was obtained by reducing the population of vibrationally excited H2 [H2 (v≥4)] at low and mid latitudes to around 25% of the value originally proposed [4], which in turn affects by the same amount the rate of charge exchange between H+ and H2 (v≥4). This leads to an overall increase in ionospheric densities, which in turn enhances ion drag at low to mid latitudes to a critical level which leads to a break-up of the pole-toequator Hadley cell and thus breaks up the return flow of energy from equator to pole, preventing equatorial cooling [1] from happening.

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