The lower ionosphere of Titan

Details The lower ionosphere of Titan The lower ionosphere of Titan

Jul 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976icar...28..367c&link_type=abstract

Icarus, vol. 28, July 1976, p. 367-378.

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21

Atmospheric Ionization, Cosmic Rays, Ionospheric Electron Density, Ionospheric Ion Density, Lower Ionosphere, Titan, Abundance, Astronomical Models, Atmospheric Chemistry, Atmospheric Models, Hydrogen, Methane, Molecular Ions, Reaction Kinetics

Scientific paper

Ionization of the atmosphere of Titan by galactic cosmic rays is a very significant process throughout the altitude range from 100 to 400 km. An approximate form of the Boltzmann equation for cosmic-ray transport has been used to obtain local ionization rates. Models of both ion and neutral chemistry have been employed to compute electron and ion density profiles for three different values of the H2/CH4 abundance ratio. The peak electron density is of the order of 1000 per cu cm. The most abundant positive ions are C2/H9(+) and C3H9(+), while the predicted densities of the negative ions H(-) and CH3(-) are very small (less than one ten-thousandth that of the positive ions). It is suggested that inclusion of the ion chemistry is important in the computation of the H and CH3 density profiles in the lower ionosphere.

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