Examining Titan’s atmospheric conductivity profile using Cassini radio occultations

Details Examining Titan’s atmospheric conductivity profile using Cassini radio occultations Examining Titan’s atmospheric conductivity profile using Cassini radio occultations

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p51c1137i&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P51C-1137

Physics

[2431] Ionosphere / Ionosphere/Magnetosphere Interactions, [2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions, [6281] Planetary Sciences: Solar System Objects / Titan

Scientific paper

We present a study investigating the atmosphere of Titan using radio occultation measurements from Cassini’s Radio Science Subsystem (RSS). While previous studies have examined the ionospheric profile above 400 km using Cassini RSS observations, and below 80 km using observations from the Huygens probe, a definitive conductivity profile at all altitudes and representing several latitudes and local times has yet to be published. There are challenges in processing Cassini radio occultation data below 400 km to study conductivity that include resolving and removing the effect of the neutral atmosphere, since the ratio of neutral to charged particles increases below that altitude. We will be surveying the multi-frequency radio occultations at Titan in search of the dispersive behavior characteristic of charged particles in the lower atmosphere. Our work employs a method previously used on Magellan data at Venus to extend processing of available Cassini occultation data to the surface. This will provide better atmospheric Schumann resonance cavity model constraints, as well as enable more complete studies of the structure of the ionosphere, its interactions with Saturn's magnetosphere, and further our understanding of the role and distribution of aerosols in Titan’s atmosphere. Schumann resonance consists of EM radiation propagating at the atmospheric cavity's resonant frequencies and it was observed for the first time on another planetary body during Huygens' descent on Titan. Modeling of Titan's cavity can shed light on characterizing a suspected underground liquid ocean and a possible radiative source, such as interactions between ionosphere and Saturn's magnetosphere. Also, characteristics of charged particles associated with the thick organic aerosol haze in Titan's atmosphere can be better constrained by a full atmospheric conductivity profile.

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