Photoelectron transport at Titan, Saturn, and Earth: comparative approach

Details Photoelectron transport at Titan, Saturn, and Earth: comparative approach Photoelectron transport at Titan, Saturn, and Earth: comparative approach

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsa31a..05g&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SA31A-05

Physics

2423 Ionization Mechanisms, 2479 Solar Radiation And Cosmic Ray Effects, 5729 Ionospheres (2459), 6207 Comparative Planetology, 6275 Saturn

Scientific paper

Solar irradiance in the extreme ultra-violet and X-ray spectral range is a major source of variability in planetary upper atmospheres through photoionization and heating processes. The induced photoelectrons have enough energy to also interact with the atmospheric population. Their transport is important for ionospheric densities and temperatures. As support of the on-going Cassini mission we recently upgraded the version of Titan's multistream electron transport model and adopted it to the atmosphere of Saturn. The goals of such calculations, unprecedented for Saturn, are to compute the electron/ion production rates induced by energetic electrons and the heating rate associated with the energy transfer between suprathermal electrons and ionospheric electrons. We will discuss how sensitive these quantities are with solar activity and compare solar-induced to photoelectron-induced electron productions. Saturn and its largest moon, Titan, do not share the same atmospheric neutral species, whereas Earth and Titan have similar atmospheric constituents at different distances from the Sun. Therefore comparing the transport of photoelectrons between these three bodies, primary goal of this study, is of particular interest.

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