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K. A. Rages (SETI Institute), S. Lebonnois (Laboratoire de Météorologie Dynamique), C. P. McKay (NASA Ames)
We model the photochemical production of hydrocarbons at low latitudes in Jupiter's stratosphere, including both aliphatic and aromatic polymers, and the growth and vertical transport of the resulting hazes. Our photochemical model is based on one previously used for Titan studies, with Jupiter's basic atmospheric characteristics derived from Gladstone {\em et al.} (1996). The modeled stratospheric composition compares well with available observations. The production of hydrocarbon polymers is evaluated from this composition, using a parameterization similar to that used for Titan (Lebonnois {\em et al.} 2002). The haze microphysics code used includes growth through coagulation from an initial distribution of very small particles given by the photochemical production profile, and vertical transport due to sedimentation and eddy diffusion. We calculate a total hydrocarbon mass production rate (for species derived from up to 20 C2H2 molecules) of order 10-15 g cm-2 s-1, with production concentrated between 0.3 and 10 mbar. The vertical extinction profile of the resulting haze will be compared with the vertical extinction profile observed by Galileo at 9\arcdeg N latitude.
Gladstone, G.R. {\em et al.} 1996. Icarus 119, 1-52. \\ Lebonnois, S. {\em et al.} 2002. Icarus 159, 505-517.
This work was funded through the NASA Planetary Atmospheres program.
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Bulletin of the American Astronomical Society, 35 #4
© 2003. The American Astronomical Soceity.