Modeling Hydrocarbons in the Atmosphere of Neptune and Comparison with Spitzer Observations

Details Modeling Hydrocarbons in the Atmosphere of Neptune and Comparison with Spitzer Observations Modeling Hydrocarbons in the Atmosphere of Neptune and Comparison with Spitzer Observations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p41a0209z&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #P41A-0209

Physics

0300 Atmospheric Composition And Structure, 0317 Chemical Kinetic And Photochemical Properties, 5405 Atmospheres (0343, 1060), 5704 Atmospheres (0343, 1060), 5709 Composition (1060)

Scientific paper

Recent observations made by the IRS instrument onboard Spitzer provide new constraints on the abundances of hydrocarbons in the atmosphere of Neptune. A one-dimensional, diurnally averaged photochemical model has been used to simulate the Spitzer results. We show that the molar fractions of complex hydrocarbons, such as benzene (C6H6), are extremely sensitive to the prescribed eddy diffusion profile, but simple hydrocarbons like ethane (C2H6) and acetylene (C2H2) are less sensitive to the eddy diffusivity. For example, reducing the eddy coefficients by a factor of 5 would enhance hydrocarbon abundances such as C4H2, CH3C2H, and C6H6 by more than an order of magnitude. In order to give the best fit to the methane data from Spitzer, we must enhance the concentration of methane at lower boundary over that given by Moses et al (2005). A sensitivity study with respect to the changes of eddy mixing, selected chemical reactions and CH4 concentration at the lower boundary will be presented.

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