The CH4 Density in the Upper Atmosphere of Titan

Details The CH4 Density in the Upper Atmosphere of Titan The CH4 Density in the Upper Atmosphere of Titan

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002icar..158..191l&link_type=abstract

Icarus, Volume 158, Issue 1, p. 191-198.

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Scientific paper

Previous modeling by Banaszkiewicz et al. (2000a,b) showed that the CH4 thermospheric mixing ratio on Titan could vary as much as 35-40% due to ion-neutral chemical reactions. A new vertical methane profile has been computed by simultaneously modifying the stratospheric methane mixing ratio and the K(z) previously considered by Lara et al. (1996) and Banaszkiewicz et al. (2000a,b). A satisfactory fit of the methane thermospheric abundance and stratospheric mixing ratio of other minor constituents is achieved by placing the homopause at ~1000 km and increasing the methane stratospheric mixing ratio (qCH4) up to 3.8%. The new proposed eddy diffusion coefficient steadily rises from 1×107 cm2 s-1 at 700 km to 1×1010 cm2 s-1 at 1500 km, whereas the stratospheric values are in the range (4-20)×103 cm2 s-1. Other likely ionization sources that can influence the methane distribution are (i) a metallic ion layer produced by micrometeoroid infall and (ii) frequent X-rays solar flares. Analysis of the effects of these ionization sources on the methane distribution indicates that, unlike previously assumed, CH4 can suffer considerable variations. These variations, although proved in this work, must be cautiously regarded since several assumptions have to be made on the rate of N2 and CH4 ionization by the processes previously mentioned. Hence, these results are only indicative of methane sensitivity to ionospheric chemistry.

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