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Models of cloud condensation under thermodynamic equilibrium in planetary atmospheres are useful for several reasons. These equilibrium cloud condensation models (ECCMs) calculate the wet adiabatic lapse rate, determine saturation-limited mixing ratios of condensing species, calculate the stabilizing effect of latent heat release and molecular weight stratification, and locate cloud base levels. Many...
Ethylene (C 2 H 4 ) emission has been measured in the poles and equator of Jupiter. The 949 cm −1 spectra were recorded with a high resolution spectrometer at the McMath–Pierce telescope at Kitt Peak in October–November 1998 and at the Infrared Telescope Facility at Mauna Kea in June 2000. C 2 H 4 is an important product of methane chemistry in the outer planets...
We report here the first detection of mono-deuterated acetylene (acetylene-d1, C 2 HD) in Titan's atmosphere from the presence of two of its emission bands at 678 and 519 cm −1 as observed in CIRS spectral averages of nadir and limb observations taken between July 2004 and mid-2007. By using new laboratory spectra for this molecule, we were able to derive its abundance at different...
We have analyzed data recorded by the Composite Infrared Spectrometer (CIRS) aboard the Cassini spacecraft during the Titan flybys T0–T10 (July 2004–January 2006). The spectra characterize various regions on Titan from 70° S to 70° N with a variety of emission angles. We study the molecular signatures observed in the mid-infrared CIRS detector arrays (FP3 and FP4, covering roughly the 600–1500 cm...
Limb spectra recorded by the Composite InfraRed Spectrometer (CIRS) on Cassini provide information on abundance vertical profiles of C 2 H 2 , C 2 H 4 , C 2 H 6 , CH 3 C 2 H, C 3 H 8 , C 4 H 2 , C 6 H 6 and HCN, along with the temperature profiles in Titan's atmosphere. We analyzed two sets...
We have performed high-resolution spectral observations at mid-infrared wavelengths of C 2 H 6 (12.16 μm), and C 2 H 2 (13.45 μm) on Saturn. These emission features probe the stratosphere of the planet and provide information on the hydrocarbon photochemical processes taking place in that region of the atmosphere. The observations were performed using our cryogenic...
We have performed high-resolution spectral observations at mid-infrared wavelengths of CH 4 (8.14 μm), C 2 H 6 (12.16 μm), and C 2 H 2 (13.45 μm) on Jupiter. These emission features probe the stratosphere of the planet and provide information on the carbon-based photochemical processes taking place in that region of the atmosphere. The observations were performed...
Abstract. Ingress and egress Voyager 2 ultraviolet spectrometer (UVS) solar occultation lightcurves at wavelengths longward of hi Lyman α acquired during the Neptune encounter are compared with one-dimensional methane photochemical-transport models to infer hydrocarbon abundances and the strength of eddy mixing in the stratosphere. Previous modeling of the 125-140 nm lightcurves indicated eddy mixing...
Recently the rate constants of the reactions C 2 H 3 + H 2 → C 2 H 4 + H and C 2 H 3 + H → products have been measured by more direct methods than used previously. The new determination for the rate constant of C 2 H 3 + H 2 is lower by a factor of 1000 at room temperature than the rate used by Allenet al. in their methane...
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